id string | problem_number string | slug string | title string | statement string | plain_statement string | precise_statement string | category string | category_number int64 | category_name string | subcategory string | secondary_categories list | question_type string | object_classes list | object_scope string | population_scope string | scales list | epochs list | wavelengths_and_messengers list | facilities_or_surveys list | observables list | inferred_properties list | selection_effects list | systematic_uncertainties list | degeneracies list | status string | published bool | evidence_state string | consensus_state string | status_last_checked timestamp[s] | status_justification string | verification_mode string | verification_horizon string | falsifiability_or_discriminant string | current_best_bounds_or_constraints string | competing_models list | resolution_criteria list | why_it_matters string | background_needed string | difficulty_level int64 | difficulty_rationale string | is_gold_seed bool | set_id int64 | sources list | related_problem_ids list | duplicate_of null | cross_domain_links list | tags list | rejection_code string | curation_notes string | version string | created_at timestamp[s] | updated_at timestamp[s] |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
UAST-000001 | UAST-000001 | uast-000001-energy-scale-of-cosmic-inflation-and-primordial-tensor-to-scalar-ratio-r | Energy Scale of Cosmic Inflation and Primordial Tensor-to-Scalar Ratio r | Did cosmic inflation generate a detectable background of primordial tensor perturbations, and what is the value of the tensor-to-scalar ratio r and energy scale V^{1/4} encoded in degree-scale cosmic microwave background B-mode polarization? | Did the early universe undergo inflation at an energy scale high enough to leave a detectable gravitational-wave imprint in the polarization of the cosmic microwave background? | Across multipoles 2 <= ell <= 200 of the cosmic microwave background polarization field, what is the amplitude r = A_t / A_s of primordial tensor modes at pivot scale k_* = 0.05 Mpc^{-1} after separating Galactic thermal dust and synchrotron foregrounds and delensing late-time gravitational E-to-B conversion? | cosmology_early_universe | 1 | Cosmology and the Early Universe | inflation_and_primordial_initial_conditions | [] | value_or_bound | [
"cosmic_background",
"early_universe",
"large_scale_structure"
] | population_level | Astrophysical systems in inflation and primordial initial conditions | [
"cosmological_horizon",
"gpc",
"10_to_100_mpc"
] | [
{
"name": "inflation_and_recombination",
"redshift_min": 1100,
"redshift_max": null,
"lookback_time_gyr_min": 13.78,
"lookback_time_gyr_max": 13.8
}
] | [
"cmb_mm_submm",
"optical",
"near_ir",
"radio_cm_m_lowfreq"
] | [
"Planck",
"JWST",
"DESI",
"Simons Observatory",
"CMB-S4"
] | [
"CMB BB angular power spectrum C_ell^{BB}",
"multi-frequency polarized dust and synchrotron SED",
"CMB lensing convergence kappa"
] | [
"tensor-to-scalar ratio r",
"inflationary energy scale V^{1/4}",
"inflaton field excursion Delta phi / M_Pl"
] | [
"sky-fraction mask exclusion of high-latitude Galactic dust filaments"
] | [
"spatially varying Galactic dust spectral index beta_d and temperature T_d",
"instrumental beam polarization leakage and HWP systematics",
"delensing residual variance"
] | [
"primordial tensor B-modes versus non-Gaussian polarized Galactic dust residuals and chiral axion-gauge field B-modes"
] | open | true | partial_observational_constraint | open_consensus | 2026-10-16T00:00:00 | BICEP/Keck and Planck observations constrain r < 0.036 (95% CL) without a detection, leaving open whether single-field Starobinsky/alpha-attractor models (r ~ 0.003-0.004) or low-scale inflation held in the early universe. | survey_statistical | decade_scale | Multi-frequency degree-scale and reionization-bump B-mode polarization measurements from Simons Observatory, LiteBIRD, and CMB-S4 reaching sigma(r) <= 5 x 10^{-4} with independent cross-frequency dust separation and >70% delensing. | Current observations from Planck, JWST, DESI constrain tensor-to-scalar ratio r, but systematic uncertainties in spatially varying Galactic dust spectral index beta_d and temperature prevent a definitive resolution. | [
"Baseline astrophysical mechanism in inflation and primordial initial conditions constrained by Planck, JWST",
"Alternative non-equilibrium, feedback, or multi-component physical model for Energy Scale of Cosmic Inflation and Primordial Tensor-to-Scalar Ratio"
] | [
"High-significance multi-wavelength or dynamical measurement of CMB BB angular power spectrum C_ell^{BB} using Planck, JWST, DESI.",
"Breaking the model degeneracy between primordial tensor B-modes versus non-Gaussian polarized Galactic dust residuals and chiral to better than 3-5 sigma."
] | Resolving this question in Cosmology and the Early Universe is essential for calibrating tensor-to-scalar ratio r and testing fundamental astrophysical theory. | Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference. | 4 | BICEP/Keck and Planck observations constrain r < 0.036 (95% CL) without a detection, leaving open whether single-field Starobinsky/alpha-attractor models (r ~ 0.003-0.004) or low-scale inflation held in the early universe. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "New Messengers and New Physics: Windows on the Dynamic Universe, Priority Area: New Windows on the Dynamic Universe (Inflation)",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-002319",
"citatio... | [
"UAST-000002",
"UAST-000018",
"UAST-000019",
"UAST-000020",
"UAST-000021",
"UAST-000022",
"UAST-000023",
"UAST-000102",
"UAST-000103",
"UAST-000104",
"UAST-000105",
"UAST-000106",
"UAST-000107",
"UAST-000108",
"UAST-000109",
"UAST-005514",
"UAST-005525",
"UAST-005551"
] | null | [] | [
"cosmology_early_universe",
"inflation_and_primordial_initial_conditions",
"cosmic inflation",
"primordial gravitational waves",
"CMB B-mode polarization"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000002 | UAST-000002 | uast-000002-abundance-and-luminosity-function-of-unexpectedly-uv-bright-galaxies-at-redshifts-z-1 | Abundance and Luminosity Function of Unexpectedly UV-Bright Galaxies at Redshifts z > 10 in JWST Surveys | What physical mechanism explains the high number density of ultraviolet-luminous galaxies observed by JWST at redshifts 10 <= z <= 14 compared with pre-JWST constant star-formation-efficiency LambdaCDM extrapolations? | Why has the James Webb Space Telescope found so many bright galaxies in the first 300 to 500 million years after the Big Bang compared with standard galaxy formation expectations? | In the rest-frame 1500 Angstrom UV luminosity function Phi(M_UV, z) at 10 <= z <= 14 measured by JWST NIRCam and NIRSpec, what combination of elevated feedback-free star formation efficiency epsilon_*, stochastic bursty star formation, top-heavy initial mass function, reduced dust attenuation, or early AGN contribution... | cosmology_early_universe | 1 | Cosmology and the Early Universe | inflation_and_primordial_initial_conditions | [] | mechanism | [
"cosmic_background",
"early_universe",
"large_scale_structure"
] | population_level | Astrophysical systems in inflation and primordial initial conditions | [
"cosmological_horizon",
"gpc",
"10_to_100_mpc"
] | [
{
"name": "inflation_and_recombination",
"redshift_min": 1100,
"redshift_max": null,
"lookback_time_gyr_min": 13.78,
"lookback_time_gyr_max": 13.8
}
] | [
"cmb_mm_submm",
"optical",
"near_ir",
"radio_cm_m_lowfreq"
] | [
"Planck",
"JWST",
"DESI",
"Simons Observatory",
"CMB-S4"
] | [
"rest-UV luminosity function Phi(M_UV, z)",
"NIRSpec spectroscopic redshifts and Balmer/UV line ratios",
"ALMA far-infrared dust continuum"
] | [
"halo-scale star formation efficiency epsilon_*",
"star formation burstiness amplitude sigma_UV",
"stellar initial mass function slope",
"stellar mass M_*"
] | [
"Eddington bias boosting intrinsically faint stochastic starbursts above flux-limited NIRCam thresholds",
"cosmic variance across small deep-field footprints"
] | [
"photometric redshift interloper contamination before NIRSpec confirmation",
"stellar population synthesis mass-to-light ratio assumptions"
] | [
"high average star formation efficiency versus high short-timescale UV luminosity scatter versus top-heavy IMF"
] | open | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | Spectroscopically confirmed galaxies up to z ~ 14.32 (JADES-GS-z14-0) demonstrate that the bright-end UV excess is real, but current rest-UV/optical spectra do not uniquely separate bursty star-formation duty cycles from feedback-free high efficiency or IMF variations. | survey_statistical | near_term_1_to_5_years | Wide-area JWST + Roman spectroscopic surveys combined with ALMA dynamical mass and dust constraints and rest-optical H-alpha/continuum duty-cycle measurements across a representative sample of z > 10 galaxies. | Current observations from Planck, JWST, DESI constrain halo-scale star formation efficiency epsilon_*, but systematic uncertainties in photometric redshift interloper contamination before NIRSpec confirmat prevent a definitive resolution. | [
"Baseline astrophysical mechanism in inflation and primordial initial conditions constrained by Planck, JWST",
"Alternative non-equilibrium, feedback, or multi-component physical model for Abundance and Luminosity Function of Unexpectedly UV-Bright Galaxies a"
] | [
"High-significance multi-wavelength or dynamical measurement of rest-UV luminosity function Phi(M_UV, z) using Planck, JWST, DESI.",
"Breaking the model degeneracy between high average star formation efficiency versus high short-timescale UV luminosity scatter v to better than 3-5 sigma."
] | Resolving this question in Cosmology and the Early Universe is essential for calibrating halo-scale star formation efficiency epsilon_* and testing fundamental astrophysical theory. | Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference. | 3 | Spectroscopically confirmed galaxies up to z ~ 14.32 (JADES-GS-z14-0) demonstrate that the bright-end UV excess is real, but current rest-UV/optical spectra do not uniquely separate bursty star-formation duty cycles from feedback-free high efficiency or IMF variations. | true | 0 | [
{
"source_id": "SRC-AST-000020",
"support_type": "direct_open_question",
"locator": "Section 2: Early Galaxy Assembly and the UV Luminosity Function, Open Question 1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-013659",
"citation": "Cueto et al. (2024, A&A 686, A138 (2024))"... | [
"UAST-000001",
"UAST-015632",
"UAST-006642",
"UAST-011557"
] | null | [] | [
"cosmology_early_universe",
"inflation_and_primordial_initial_conditions",
"z > 10 UV-bright galaxies",
"cosmic dawn star formation",
"UV luminosity function"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000020). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000003 | UAST-000003 | uast-000003-physical-origin-of-the-hubble-constant-tension-between-early-universe-cmb-bao-inferen | Physical Origin of the Hubble Constant Tension Between Early-Universe CMB+BAO Inference and Local Distance Ladders | Does the discrepancy between the Hubble constant H_0 inferred from Planck CMB and BAO sound-horizon measurements under LambdaCDM and the local Cepheid-calibrated Type Ia supernova distance ladder (SH0ES) arise from beyond-LambdaCDM early-universe physics or from unmodeled distance-ladder systematics? | Why do measurements of the cosmic expansion rate from the early universe disagree with measurements from nearby stars and supernovae? | Between early-universe sound-horizon determinations (Planck + ACT + SPT + DESI BAO giving H_0 = 67.4-68.0 km s^{-1} Mpc^{-1}) and local distance-ladder calibrations of Type Ia supernovae (SH0ES Cepheids giving H_0 = 73.0 +- 1.0 km s^{-1} Mpc^{-1} versus CCHP TRGB/JAGB calibrations), what accounts for the offset in infe... | dark_matter_dark_energy_fundamental_cosmology | 2 | Dark Matter, Dark Energy, and Fundamental Cosmology | primordial_black_holes_and_exotic_relics | [] | tension_resolution | [
"dark_sector",
"galaxy",
"large_scale_structure"
] | population_level | Astrophysical systems in primordial black holes and exotic relics | [
"kpc",
"mpc",
"gpc"
] | [
{
"name": "late_time_acceleration_and_halo_assembly",
"redshift_min": 0,
"redshift_max": 3,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 11.5
}
] | [
"optical",
"near_ir",
"gravitational_wave",
"x_ray"
] | [
"Vera C. Rubin Observatory LSST",
"Euclid",
"DESI",
"Nancy Grace Roman Space Telescope",
"HST"
] | [
"Cepheid period-luminosity relations",
"TRGB and JAGB tip magnitudes in JWST NIRCam",
"SNe Ia Hubble diagram",
"CMB acoustic peak angular scale theta_*"
] | [
"present-day Hubble constant H_0",
"comoving sound horizon r_d",
"absolute SNe Ia magnitude M_B"
] | [
"host-galaxy selection and crowding in Cepheid vs TRGB/JAGB calibrator samples"
] | [
"Cepheid metallicity and dust-law slope R_V calibration",
"TRGB tip-detection smoothing and zero-point anchoring",
"peculiar velocity bulk-flow corrections"
] | [
"early dark energy reducing r_d versus local distance-scale zero-point shift Delta M_B"
] | open | true | partial_observational_constraint | open_consensus | 2026-10-16T00:00:00 | SH0ES HST+JWST Cepheid measurements maintain a ~5 sigma tension with Planck LambdaCDM, whereas CCHP JWST TRGB and JAGB analyses yield H_0 ~ 69.9 +- 1.7 km s^{-1} Mpc^{-1}, leaving the role of calibrator systematics versus early-universe physics unresolved. | multimessenger | decade_scale | Sub-percent distance-ladder-independent H_0 determinations from gravitational-wave standard sirens and strong-lensing time delays, alongside converged JWST Cepheid/TRGB/JAGB calibrations across >=40 SNe Ia hosts. | Current observations from Vera C. Rubin Observatory LSST, Euclid, DESI constrain present-day Hubble constant H_0, but systematic uncertainties in Cepheid metallicity and dust-law slope R_V calibration prevent a definitive resolution. | [
"Baseline astrophysical mechanism in primordial black holes and exotic relics constrained by Vera C. Rubin Observatory LSST, Euclid",
"Alternative non-equilibrium, feedback, or multi-component physical model for Physical Origin of the Hubble Constant Tension Between Early-Universe "
] | [
"High-significance multi-wavelength or dynamical measurement of Cepheid period-luminosity relations using Vera C. Rubin Observatory LSST, Euclid, DESI.",
"Breaking the model degeneracy between early dark energy reducing r_d versus local distance-scale zero-point shift Delta M_B to better than 3-5 sigma."
] | Resolving this question in Dark Matter, Dark Energy, and Fundamental Cosmology is essential for calibrating present-day Hubble constant H_0 and testing fundamental astrophysical theory. | Dark matter halo dynamics, weak and strong gravitational lensing formalism, modified gravity screening theories, and dark energy equation-of-state phenomenology. | 4 | SH0ES HST+JWST Cepheid measurements maintain a ~5 sigma tension with Planck LambdaCDM, whereas CCHP JWST TRGB and JAGB analyses yield H_0 ~ 69.9 +- 1.7 km s^{-1} Mpc^{-1}, leaving the role of calibrator systematics versus early-universe physics unresolved. | true | 0 | [
{
"source_id": "SRC-AST-000014",
"support_type": "direct_open_question",
"locator": "Section 2: The Hubble Constant Tension, Tension 1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-001315",
"citation": "Poulin et al. (2024, arXiv (astro-ph.CO))",
"support_type": "explicit... | [
"UAST-000004",
"UAST-000024",
"UAST-000025",
"UAST-000026",
"UAST-000027",
"UAST-000028",
"UAST-000029",
"UAST-000374",
"UAST-000375",
"UAST-000376",
"UAST-000377",
"UAST-000378",
"UAST-000379",
"UAST-000380",
"UAST-000381",
"UAST-004510",
"UAST-004169",
"UAST-004866"
] | null | [] | [
"dark_matter_dark_energy_fundamental_cosmology",
"primordial_black_holes_and_exotic_relics",
"Hubble constant H_0",
"local distance ladder",
"cosmic sound horizon r_d"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000014). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000004 | UAST-000004 | uast-000004-dynamical-evolution-of-dark-energy-equation-of-state-w-z-suggested-by-desi-bao-type-i | Dynamical Evolution of Dark Energy Equation of State w(z) Suggested by DESI BAO + Type Ia Supernova Combinations | Is cosmic acceleration driven by a time-independent cosmological constant (w = -1), or does dark energy evolve dynamically with redshift (w_0 > -1, w_a < 0) as hinted by joint DESI baryon acoustic oscillation, CMB, and Type Ia supernova analyses? | Is dark energy a fixed cosmological constant, or is its strength changing over cosmic time? | In the Chevallier-Polarski-Linder parameterization w(a) = w_0 + w_a(1 - a) fitted to transverse and radial BAO distances D_M(z)/r_d and D_H(z)/r_d across 0.1 < z < 2.5 together with CMB and SNe Ia (Pantheon+, Union3, DES-SN5YR), does the preference for w_0 > -1 and w_a < 0 reflect dynamical dark energy or supernova red... | dark_matter_dark_energy_fundamental_cosmology | 2 | Dark Matter, Dark Energy, and Fundamental Cosmology | primordial_black_holes_and_exotic_relics | [] | population_evolution | [
"dark_sector",
"galaxy",
"large_scale_structure"
] | population_level | Astrophysical systems in primordial black holes and exotic relics | [
"kpc",
"mpc",
"gpc"
] | [
{
"name": "late_time_acceleration_and_halo_assembly",
"redshift_min": 0,
"redshift_max": 3,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 11.5
}
] | [
"optical",
"near_ir",
"gravitational_wave",
"x_ray"
] | [
"Vera C. Rubin Observatory LSST",
"Euclid",
"DESI",
"Nancy Grace Roman Space Telescope",
"HST"
] | [
"anisotropic BAO distance ratios D_M(z)/r_d and D_H(z)/r_d",
"SNe Ia luminosity distance modulus mu(z)",
"full-shape galaxy power spectrum P(k)"
] | [
"dark energy equation-of-state parameters (w_0, w_a)",
"matter density parameter Omega_m"
] | [
"Malmquist and host-mass step selection biases in high-redshift photometric SNe Ia compilations"
] | [
"photometric calibration offsets between low-z anchor SNe and high-z rolling survey SNe",
"prior volume effects in (w_0, w_a) parameterization"
] | [
"evolving dark energy w(z) versus spatial curvature Omega_k, neutrino mass sum m_nu, and SNe Ia progenitor evolution"
] | open | true | partial_observational_constraint | open_consensus | 2026-10-16T00:00:00 | DESI 2024 BAO + CMB + SNe Ia shows a 2.5-3.9 sigma preference for (w_0 > -1, w_a < 0) depending on the supernova compilation used (Pantheon+, Union3, DES-SN5YR), which has not yet reached the 5-sigma discovery threshold or excluded supernova calibration systematics. | multimessenger | decade_scale | Full 5-year DESI spectroscopic BAO + RSD dataset combined with Euclid, Roman, and Rubin LSST homogeneously calibrated SNe Ia and weak-lensing growth measurements. | Current observations from Vera C. Rubin Observatory LSST, Euclid, DESI constrain dark energy equation-of-state parameters (w_0, w_a), but systematic uncertainties in photometric calibration offsets between low-z anchor SNe and high-z ro prevent a definitive resolution. | [
"Baseline astrophysical mechanism in primordial black holes and exotic relics constrained by Vera C. Rubin Observatory LSST, Euclid",
"Alternative non-equilibrium, feedback, or multi-component physical model for Dynamical Evolution of Dark Energy Equation of State w(z) Suggested by"
] | [
"High-significance multi-wavelength or dynamical measurement of anisotropic BAO distance ratios D_M(z)/r_d and D_H(z)/r_d using Vera C. Rubin Observatory LSST, Euclid, DESI.",
"Breaking the model degeneracy between evolving dark energy w(z) versus spatial curvature Omega_k, neutrino mass sum m_nu, and SN to bette... | Resolving this question in Dark Matter, Dark Energy, and Fundamental Cosmology is essential for calibrating dark energy equation-of-state parameters (w_0, w_a) and testing fundamental astrophysical theory. | Dark matter halo dynamics, weak and strong gravitational lensing formalism, modified gravity screening theories, and dark energy equation-of-state phenomenology. | 4 | DESI 2024 BAO + CMB + SNe Ia shows a 2.5-3.9 sigma preference for (w_0 > -1, w_a < 0) depending on the supernova compilation used (Pantheon+, Union3, DES-SN5YR), which has not yet reached the 5-sigma discovery threshold or excluded supernova calibration systematics. | true | 0 | [
{
"source_id": "SRC-AST-000019",
"support_type": "direct_open_question",
"locator": "Section 5: Dark Energy and Modified Gravity Constraints, Result w0-wa",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-000974",
"citation": "Favale et al. (2025, Mon Not R Astron Soc (2026))",
... | [
"UAST-000003",
"UAST-004169",
"UAST-004275",
"UAST-003852"
] | null | [] | [
"dark_matter_dark_energy_fundamental_cosmology",
"primordial_black_holes_and_exotic_relics",
"dark energy equation of state w(z)",
"baryon acoustic oscillations",
"cosmic expansion history"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000019). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000005 | UAST-000005 | uast-000005-spatial-distribution-and-baryon-partition-of-the-warm-hot-intergalactic-medium-across | Spatial Distribution and Baryon Partition of the Warm-Hot Intergalactic Medium Across Cosmic Web Filaments | How are the low-redshift 'missing baryons' partitioned in temperature, density, and metallicity between the diffuse warm-hot intergalactic medium (WHIM, 10^5-10^7 K) in cosmic web filaments and the outer circumgalactic halos of galaxies? | Where exactly does normal matter reside between galaxies in the modern universe, and how much of it is in cosmic web filaments versus extended galaxy halos? | At redshifts z < 1, what fraction of the cosmic baryon budget Omega_b resides in unvirialized cosmic-web filaments versus virialized halo gas as a function of overdensity delta_b and temperature T, and how do AGN and supernova outflows heat and enrich this gas? | large_scale_structure_igm_cosmic_web | 3 | Large-Scale Structure, Intergalactic Medium, and Cosmic Web | intergalactic_medium_and_lya_forest | [] | object_nature | [
"large_scale_structure",
"intergalactic_medium",
"circumgalactic_medium",
"galaxy_cluster"
] | population_level | Astrophysical systems in intergalactic medium and lya forest | [
"kpc",
"mpc",
"10_to_100_mpc"
] | [
{
"name": "cosmic_noon_to_present",
"redshift_min": 0,
"redshift_max": 5,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.6
}
] | [
"uv",
"optical",
"x_ray",
"cmb_mm_submm",
"radio_cm_m_lowfreq"
] | [
"DESI",
"XRISM",
"eROSITA",
"ACT",
"SPT-3G"
] | [
"fast radio burst dispersion measure DM(z)",
"O VII and O VIII X-ray absorption/emission lines",
"thermal and kinematic Sunyaev-Zel'dovich profiles"
] | [
"baryon mass fraction f_WHIM",
"electron density profile n_e(r)",
"IGM metallicity Z_IGM and temperature T_WHIM"
] | [
"sightline bias toward overdense galaxy groups in stacked tSZ/X-ray filament analyses"
] | [
"host-galaxy and Milky Way halo DM subtraction in localized FRB samples",
"non-equilibrium ionization and clumping factor C = <n_e^2>/<n_e>^2"
] | [
"electron column density versus gas metallicity in X-ray O VII/O VIII absorption"
] | partially_solved | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | Localized fast radio bursts (Macquart relation) and stacked tSZ/X-ray filaments confirm that the total cosmic baryon density Omega_b is present at low redshift, but the radial partition between extended circumgalactic halos and diffuse intergalactic filaments remains model-dependent. | survey_statistical | near_term_1_to_5_years | Joint tomography using >=1,000 host-localized FRBs (DSA-2000, CHIME Outriggers, SKA), high-resolution X-ray microcalorimeter absorption spectra (XRISM, NewAthena, Arcus), and CMB-S4/Simons Observatory kSZ profiling. | Current observations from DESI, XRISM, eROSITA constrain baryon mass fraction f_WHIM, but systematic uncertainties in host-galaxy and Milky Way halo DM subtraction in localized FRB samples prevent a definitive resolution. | [
"Baseline astrophysical mechanism in intergalactic medium and lya forest constrained by DESI, XRISM",
"Alternative non-equilibrium, feedback, or multi-component physical model for Spatial Distribution and Baryon Partition of the Warm-Hot Intergalacti"
] | [
"High-significance multi-wavelength or dynamical measurement of fast radio burst dispersion measure DM(z) using DESI, XRISM, eROSITA.",
"Breaking the model degeneracy between electron column density versus gas metallicity in X-ray O VII/O VIII absorption to better than 3-5 sigma."
] | Resolving this question in Large-Scale Structure, Intergalactic Medium, and Cosmic Web is essential for calibrating baryon mass fraction f_WHIM and testing fundamental astrophysical theory. | Cosmological hydrodynamics, radiative cooling and photoionization equilibrium, X-ray and Sunyaev-Zel'dovich cluster physics, and Lyman-alpha forest statistics. | 3 | Localized fast radio bursts (Macquart relation) and stacked tSZ/X-ray filaments confirm that the total cosmic baryon density Omega_b is present at low redshift, but the radial partition between extended circumgalactic halos and diffuse intergalactic filaments remains model-dependent. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Cosmic Ecosystems: Unveiling the Drivers of Galaxy Growth, Question CE-1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-005328",
"citation": "Zhai et al. (2026, arXiv (astro-ph.CO))",
"sup... | [
"UAST-000030",
"UAST-000031",
"UAST-000032",
"UAST-000033",
"UAST-000034",
"UAST-000035",
"UAST-000576",
"UAST-000577",
"UAST-000578",
"UAST-000579",
"UAST-000580",
"UAST-000581",
"UAST-000582",
"UAST-000583",
"UAST-000584",
"UAST-008084",
"UAST-010053",
"UAST-008116"
] | null | [] | [
"large_scale_structure_igm_cosmic_web",
"intergalactic_medium_and_lya_forest",
"warm-hot intergalactic medium (WHIM)",
"cosmic web filaments",
"missing baryon budget"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000006 | UAST-000006 | uast-000006-seeding-mechanism-of-overmassive-black-holes-at-redshifts-z-6-light-population-iii-re | Seeding Mechanism of Overmassive Black Holes at Redshifts z > 6: Light Population III Remnants versus Heavy Direct-Collapse Seeds | Did the supermassive black holes of mass 10^7-10^9 M_sun observed by JWST and quasar surveys at redshifts z > 6 grow from light Population III stellar remnants (~10^2 M_sun) via sustained super-Eddington accretion, from intermediate-mass runaway cluster collapses (~10^3 M_sun), or from heavy direct-collapse black hole ... | How did the first giant black holes in the universe grow so massive in less than a billion years after the Big Bang? | For the population of broad-line AGN and quasars at 6 <= z <= 11 discovered by JWST and wide-field surveys, what initial seed mass function dN/dM_seed at z = 15-30 and Eddington duty-cycle distribution f_Edd(t) produce the observed black hole mass function and elevated M_BH / M_* ratios? | galaxies_supermassive_black_holes | 4 | Galaxies and Supermassive Black Holes | high_redshift_galaxy_formation_and_first_galaxies | [] | model_discrimination | [
"galaxy",
"agn_quasar",
"compact_object"
] | population_level | Astrophysical systems in high redshift galaxy formation and first galaxies | [
"pc",
"kpc",
"mpc"
] | [
{
"name": "first_galaxies_through_cosmic_noon",
"redshift_min": 0,
"redshift_max": 14,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 13.5
}
] | [
"near_ir",
"mid_ir",
"optical",
"mm_submm",
"x_ray",
"radio_cm_m_lowfreq"
] | [
"JWST",
"ALMA",
"Chandra",
"VLT/MUSE",
"SDSS/BOSS"
] | [
"JWST broad H-alpha/H-beta line widths and luminosities",
"black hole-to-stellar mass ratio M_BH/M_* at z = 6-10",
"LISA gravitational-wave merger rates at z > 10"
] | [
"seed mass distribution M_seed",
"time-averaged Eddington accretion ratio lambda_Edd",
"black hole occupation fraction in dwarf/high-z galaxies"
] | [
"Lauer bias and flux-limit selection favoring the highest-M_BH/M_* outliers in high-z spectroscopic samples"
] | [
"single-epoch virial black hole mass calibration uncertainties at high redshift and super-Eddington rates",
"X-ray weakness and Compton-thick obscuration in JWST 'Little Red Dots'"
] | [
"heavy initial seed mass M_seed ~ 10^5 M_sun with sub-Eddington growth versus light seed M_seed ~ 100 M_sun with episodic super-Eddington accretion"
] | open | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | JWST has revealed abundant broad-line AGN and compact 'Little Red Dots' at z = 5-10 with apparent M_BH/M_* ratios 10-100x above local relations, but virial mass systematics and lack of direct z > 10 gravitational-wave detections prevent distinguishing heavy seeds from super-Eddington light seeds. | observational_and_theoretical | decade_scale | Direct detection of black hole seed mergers at z = 10-20 with LISA, combined with reverberation mapping and X-ray/infrared spectral disentangling of z > 7 AGN with JWST, NewAthena, and ELTs. | Current observations from JWST, ALMA, Chandra constrain seed mass distribution M_seed, but systematic uncertainties in single-epoch virial black hole mass calibration uncertainties at high prevent a definitive resolution. | [
"Baseline astrophysical mechanism in high redshift galaxy formation and first galaxies constrained by JWST, ALMA",
"Alternative non-equilibrium, feedback, or multi-component physical model for Seeding Mechanism of Overmassive Black Holes at Redshifts z > 6: Light"
] | [
"High-significance multi-wavelength or dynamical measurement of JWST broad H-alpha/H-beta line widths and luminosities using JWST, ALMA, Chandra.",
"Breaking the model degeneracy between heavy initial seed mass M_seed ~ 10^5 M_sun with sub-Eddington growth versus light seed M_ to better than 3-5 sigma."
] | Resolving this question in Galaxies and Supermassive Black Holes is essential for calibrating seed mass distribution M_seed and testing fundamental astrophysical theory. | Galaxy formation and evolution, active galactic nucleus accretion and feedback physics, stellar population synthesis, and galactic dynamics. | 4 | JWST has revealed abundant broad-line AGN and compact 'Little Red Dots' at z = 5-10 with apparent M_BH/M_* ratios 10-100x above local relations, but virial mass systematics and lack of direct z > 10 gravitational-wave detections prevent distinguishing heavy seeds from super-Eddington light seeds. | true | 0 | [
{
"source_id": "SRC-AST-000011",
"support_type": "direct_open_question",
"locator": "LISA Science Objective 2: Trace the Origin and Growth of Massive Black Holes, Objective SO2",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-022601",
"citation": "Ellis et al. (2023, ApJ 964 11 ... | [
"UAST-000036",
"UAST-000037",
"UAST-000038",
"UAST-000039",
"UAST-000040",
"UAST-000041",
"UAST-000814",
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"UAST-000816",
"UAST-000817",
"UAST-000818",
"UAST-000819",
"UAST-000820",
"UAST-000821",
"UAST-000822",
"UAST-023721",
"UAST-012071",
"UAST-011713"
] | null | [] | [
"galaxies_supermassive_black_holes",
"high_redshift_galaxy_formation_and_first_galaxies",
"high-redshift supermassive black hole seeds",
"direct-collapse black holes",
"JWST broad-line AGN"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000011). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000007 | UAST-000007 | uast-000007-core-cusp-density-profiles-and-dark-subhalo-abundance-in-milky-way-ultra-faint-dwarf | Core-Cusp Density Profiles and Dark Subhalo Abundance in Milky Way Ultra-Faint Dwarf Galaxies and Stellar Streams | Do the central dark matter density profiles of ultra-faint dwarf galaxies (M_* < 10^5 M_sun) and the perturbation spectrum of cold Milky Way stellar streams match collisionless cold dark matter predictions (steep cusps and abundant 10^6-10^8 M_sun dark subhalos), or do they require self-interacting, warm, or wave-like ... | Are the centers of the faintest dwarf galaxies and the gaps in Milky Way star streams consistent with standard cold dark matter, or do they point to dark matter with new particle properties? | In Milky Way ultra-faint dwarf galaxies where supernova baryonic core formation is energetically negligible (M_*/M_halo < 10^{-4}) and along thin globular-cluster stellar streams (such as GD-1 and Pal 5), what are the inner logarithmic dark matter density slope gamma = -d ln rho / d ln r and the subhalo mass function d... | milky_way_local_group_near_field | 5 | Milky Way, Local Group, and Near-Field Cosmology | galactic_center_and_fermi_erosita_bubbles | [] | mechanism | [
"milky_way_component",
"stellar_population",
"galaxy",
"dark_sector"
] | population_level | Astrophysical systems in galactic center and fermi erosita bubbles | [
"pc",
"kpc"
] | [
{
"name": "milky_way_assembly_history",
"redshift_min": 0,
"redshift_max": 4,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.2
}
] | [
"optical",
"near_ir",
"radio_cm_m_lowfreq",
"gamma_ray",
"x_ray"
] | [
"Gaia",
"SDSS-V",
"APOGEE",
"GALAH",
"WEAVE"
] | [
"3D stellar velocity dispersions and Gaia proper motions in ultra-faint dwarfs",
"stellar stream density gaps and spur phase-space perturbations",
"strong-lensing flux-ratio and image perturbations"
] | [
"inner dark matter density slope gamma(r < 100 pc)",
"subhalo mass function dN/dM_sub at 10^6-10^8 M_sun",
"dark matter self-interaction cross section sigma/m or particle mass m_WDM"
] | [
"surface-brightness completeness limits in satellite discovery prior to Rubin LSST",
"tidal disruption of inner-halo subhalos by the Milky Way disk"
] | [
"velocity anisotropy beta(r) degeneracy in Jeans dynamical modeling",
"unresolved binary-star orbital velocity inflation",
"baryonic perturbation of streams by giant molecular clouds and the Galactic bar"
] | [
"Jeans mass-anisotropy degeneracy between a cored halo with tangential orbits and a cuspy NFW halo with radial orbits"
] | open | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | Line-of-sight velocity dispersions alone suffer from the Jeans mass-anisotropy degeneracy, and observed stream gaps in GD-1 must be separated from baryonic substructures in the Milky Way disk and halo. | observational_and_theoretical | near_term_1_to_5_years | Internal 3D plane-of-sky proper motion dispersions of >=20 ultra-faint dwarfs from Gaia + Roman + 30m-class ELTs together with Rubin LSST + Desi/Spec-S5 phase-space mapping of >=50 cold stellar streams. | Current observations from Gaia, SDSS-V, APOGEE constrain inner dark matter density slope gamma(r < 100 pc), but systematic uncertainties in velocity anisotropy beta(r) degeneracy in Jeans dynamical modeling prevent a definitive resolution. | [
"Baseline astrophysical mechanism in galactic center and fermi erosita bubbles constrained by Gaia, SDSS-V",
"Alternative non-equilibrium, feedback, or multi-component physical model for Core-Cusp Density Profiles and Dark Subhalo Abundance in Milky Way Ult"
] | [
"High-significance multi-wavelength or dynamical measurement of 3D stellar velocity dispersions and Gaia proper motions in ultra-faint dwarfs using Gaia, SDSS-V, APOGEE.",
"Breaking the model degeneracy between Jeans mass-anisotropy degeneracy between a cored halo with tangential orbits and a cuspy N to better th... | Resolving this question in Milky Way, Local Group, and Near-Field Cosmology is essential for calibrating inner dark matter density slope gamma(r < 100 pc) and testing fundamental astrophysical theory. | Galactic dynamics, action-angle phase-space modeling, stellar nucleosynthesis and chemical evolution, and Local Group near-field cosmology. | 3 | Line-of-sight velocity dispersions alone suffer from the Jeans mass-anisotropy degeneracy, and observed stream gaps in GD-1 must be separated from baryonic substructures in the Milky Way disk and halo. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Panel on Galaxies and Near-Field Cosmology, Question NFC-1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-003601",
"citation": "Yang et al. (2024, ApJ, 1001:54 (2026))",
"support_type": "e... | [
"UAST-000042",
"UAST-000043",
"UAST-000044",
"UAST-000045",
"UAST-000046",
"UAST-000047",
"UAST-001122",
"UAST-001123",
"UAST-001124",
"UAST-001125",
"UAST-001126",
"UAST-001127",
"UAST-001128",
"UAST-001129",
"UAST-001130",
"UAST-006595",
"UAST-006246",
"UAST-001136"
] | null | [] | [
"milky_way_local_group_near_field",
"galactic_center_and_fermi_erosita_bubbles",
"ultra-faint dwarf galaxies",
"Milky Way stellar streams",
"dark matter subhalo mass function"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000008 | UAST-000008 | uast-000008-relative-roles-of-magnetic-fields-supersonic-turbulence-and-stellar-feedback-in-regul | Relative Roles of Magnetic Fields, Supersonic Turbulence, and Stellar Feedback in Regulating the Low Efficiency of Molecular Cloud Star Formation | What quantitative balance among magnetohydrodynamic turbulence, magnetic flux support (mass-to-flux ratio mu_Phi), and protostellar/massive-star feedback restricts the star formation efficiency per free-fall time in giant molecular clouds to epsilon_ff ~ 1% across diverse galactic environments? | Why do giant interstellar gas clouds convert only about one percent of their mass into stars during each gravitational collapse timescale? | Across giant molecular clouds and dense clumps from local spiral disks to starburst and high-redshift environments, how do the virial parameter alpha_vir, sonic Mach number M_s, Alfvénic Mach number M_A, and radiative/momentum feedback jointly set the star formation efficiency per free-fall time epsilon_ff and the core... | ism_star_formation_astrochemistry | 6 | Interstellar Medium, Star Formation, and Astrochemistry | astrochemistry_and_complex_organic_molecules | [] | mechanism | [
"interstellar_medium",
"dust_and_ice",
"star"
] | population_level | Astrophysical systems in astrochemistry and complex organic molecules | [
"au",
"pc",
"kpc"
] | [
{
"name": "present_day_and_galactic_ism",
"redshift_min": 0,
"redshift_max": 2,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 10.4
}
] | [
"mm_submm",
"far_ir",
"mid_ir",
"radio_cm_m_lowfreq",
"uv"
] | [
"ALMA",
"JWST",
"NOEMA",
"VLA",
"ngVLA"
] | [
"Zeeman splitting and dust polarization maps",
"molecular line velocity dispersion-size relations",
"dense-gas HCN/HCO+/CO ratios and young stellar object counts"
] | [
"star formation efficiency per free-fall time epsilon_ff",
"mass-to-magnetic-flux ratio mu_Phi",
"turbulent driving scale and compressive-to-solenoidal ratio"
] | [
"evolutionary snapshot bias when inferring cloud-lifetime epsilon_ff from instantaneous YSO-to-gas ratios"
] | [
"CO-to-H2 conversion factor X_CO and HCN optical-depth variations",
"Davis-Chandrasekhar-Fermi magnetic field strength calibration uncertainties",
"radiative transfer and dust grain alignment efficiency"
] | [
"gravoturbulent fragmentation regulated by supersonic turbulence versus magnetically subcritical ambipolar-diffusion regulation"
] | open | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | Both turbulence-regulated (gravo-turbulent) and magnetically regulated models can reproduce epsilon_ff ~ 0.01 in simulations, while 3D magnetic field strengths at the prestellar core scale remain difficult to measure directly across large cloud samples. | observational_and_theoretical | near_term_1_to_5_years | High-resolution ALMA and ngVLA Zeeman + dust-polarization and kinematic surveys across thousands of cores spanning Milky Way and PHANGS extragalactic clouds, benchmarked against radiation-MHD simulations resolving 0.01 pc scales. | Current observations from ALMA, JWST, NOEMA constrain star formation efficiency per free-fall time epsilon_ff, but systematic uncertainties in CO-to-H2 conversion factor X_CO and HCN optical-depth variations prevent a definitive resolution. | [
"Baseline astrophysical mechanism in astrochemistry and complex organic molecules constrained by ALMA, JWST",
"Alternative non-equilibrium, feedback, or multi-component physical model for Relative Roles of Magnetic Fields, Supersonic Turbulence, and Stellar "
] | [
"High-significance multi-wavelength or dynamical measurement of Zeeman splitting and dust polarization maps using ALMA, JWST, NOEMA.",
"Breaking the model degeneracy between gravoturbulent fragmentation regulated by supersonic turbulence versus magnetically subcri to better than 3-5 sigma."
] | Resolving this question in Interstellar Medium, Star Formation, and Astrochemistry is essential for calibrating star formation efficiency per free-fall time epsilon_ff and testing fundamental astrophysical theory. | Magnetohydrodynamic interstellar turbulence, radiative transfer in molecular lines and dust continuum, star formation physics, and astrochemical reaction networks. | 3 | Both turbulence-regulated (gravo-turbulent) and magnetically regulated models can reproduce epsilon_ff ~ 0.01 in simulations, while 3D magnetic field strengths at the prestellar core scale remain difficult to measure directly across large cloud samples. | true | 0 | [
{
"source_id": "SRC-AST-000007",
"support_type": "direct_open_question",
"locator": "ngVLA Key Science Goal 3: Star Formation and the Interstellar Medium, KSG 3.1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-032610",
"citation": "Bertram et al. (2011, arXiv (astro-ph.SR))",
... | [
"UAST-000048",
"UAST-000049",
"UAST-000050",
"UAST-000051",
"UAST-000052",
"UAST-000053",
"UAST-001325",
"UAST-001326",
"UAST-001327",
"UAST-001328",
"UAST-001329",
"UAST-001330",
"UAST-001331",
"UAST-001332",
"UAST-001333",
"UAST-032884",
"UAST-016091",
"UAST-011510"
] | null | [] | [
"ism_star_formation_astrochemistry",
"astrochemistry_and_complex_organic_molecules",
"giant molecular clouds",
"star formation efficiency epsilon_ff",
"interstellar magnetic fields and turbulence"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000007). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000009 | UAST-000009 | uast-000009-physical-mechanism-of-common-envelope-ejection-and-orbital-shrinkage-in-interacting-b | Physical Mechanism of Common-Envelope Ejection and Orbital Shrinkage in Interacting Binary Stars | During common-envelope evolution in close binary stars, what combination of gravitational drag, hydrogen/helium ionization recombination energy, magnetohydrodynamic jets, and dust-driven winds ejects the shared stellar envelope and sets the final post-common-envelope orbital separation? | When a giant star engulfs its companion star, what physical forces eject the shared gas envelope and determine how close the two stellar cores end up? | In binary systems undergoing dynamically unstable mass transfer onto a main-sequence or compact companion, what fraction of the released orbital binding energy (alpha_CE) and internal recombination/enthalpy energy unbinds the envelope without causing a premature stellar merger, and how does this depend on donor mass M_... | stars_stellar_populations_evolution | 7 | Stars, Stellar Populations, and Stellar Evolution | binary_and_multiple_star_evolution | [] | population_evolution | [
"star",
"stellar_population",
"transient"
] | population_level | Astrophysical systems in binary and multiple star evolution | [
"1000km_to_rsun",
"au",
"pc"
] | [
{
"name": "stellar_evolution_across_metallicity",
"redshift_min": 0,
"redshift_max": 3,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 11.5
}
] | [
"optical",
"uv",
"near_ir",
"mid_ir",
"x_ray"
] | [
"Kepler",
"TESS",
"PLATO",
"Gaia",
"HST"
] | [
"post-common-envelope binary period-mass distributions",
"light curves and ejecta kinematics of luminous red novae",
"compact binary merger rate densities"
] | [
"common-envelope ejection efficiency alpha_CE",
"recombination energy thermalization fraction",
"post-infall final orbital separation a_f"
] | [
"observational bias toward short-period eclipsing post-CE white dwarf + M-dwarf binaries"
] | [
"3D radiation-hydrodynamic spatial resolution near the inspiraling companion cores",
"convective energy transport and radiation leakage timescales during hydrogen recombination"
] | [
"orbital energy conversion efficiency alpha_CE versus internal thermal/recombination energy and jet-assisted envelope removal"
] | open | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | Three-dimensional hydrodynamic simulations of the dynamical plunge typically stall before unbinding the entire envelope unless recombination energy or jets are included, leaving population synthesis models reliant on phenomenological alpha_CE prescriptions that vary by an order of magnitude. | observational_and_theoretical | near_term_1_to_5_years | 3D radiation-magnetohydrodynamic simulations spanning the dynamical plunge to thermal relaxation, tested against Rubin LSST luminous red nova transient demographics and Gaia DR4/DR5 post-CE binary populations. | Current observations from Kepler, TESS, PLATO constrain common-envelope ejection efficiency alpha_CE, but systematic uncertainties in 3D radiation-hydrodynamic spatial resolution near the inspiraling comp prevent a definitive resolution. | [
"Baseline astrophysical mechanism in binary and multiple star evolution constrained by Kepler, TESS",
"Alternative non-equilibrium, feedback, or multi-component physical model for Physical Mechanism of Common-Envelope Ejection and Orbital Shrinkage i"
] | [
"High-significance multi-wavelength or dynamical measurement of post-common-envelope binary period-mass distributions using Kepler, TESS, PLATO.",
"Breaking the model degeneracy between orbital energy conversion efficiency alpha_CE versus internal thermal/recombination energy to better than 3-5 sigma."
] | Resolving this question in Stars, Stellar Populations, and Stellar Evolution is essential for calibrating common-envelope ejection efficiency alpha_CE and testing fundamental astrophysical theory. | Stellar structure and evolution, asteroseismology, radiation-driven stellar winds, binary interaction and common-envelope hydrodynamics, and core-collapse supernova physics. | 3 | Three-dimensional hydrodynamic simulations of the dynamical plunge typically stall before unbinding the entire envelope unless recombination energy or jets are included, leaving population synthesis models reliant on phenomenological alpha_CE prescriptions that vary by an order of magnitude. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Panel on Stars, the Sun, and Stellar Populations, Question SSP-2",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-008572",
"citation": "Alonso-Álvarez et al. (2024, arXiv (astro-ph.CO))",
"s... | [
"UAST-000054",
"UAST-000055",
"UAST-000056",
"UAST-000057",
"UAST-000058",
"UAST-000059",
"UAST-001598",
"UAST-001599",
"UAST-001600",
"UAST-001601",
"UAST-001602",
"UAST-001603",
"UAST-001604",
"UAST-001605",
"UAST-001606",
"UAST-011021",
"UAST-033681",
"UAST-028507"
] | null | [] | [
"stars_stellar_populations_evolution",
"binary_and_multiple_star_evolution",
"common-envelope binary evolution",
"luminous red novae",
"close compact-object binary progenitors"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000010 | UAST-000010 | uast-000010-cold-dense-matter-equation-of-state-and-existence-of-deconfined-quark-cores-inside-ma | Cold Dense Matter Equation of State and Existence of Deconfined Quark Cores Inside Massive Neutron Stars | What is the cold supranuclear equation of state P(epsilon) inside neutron stars at densities of 2-8 times nuclear saturation density, and do massive neutron stars (~2 M_sun) contain deconfined quark matter or hyperonic cores via a first-order phase transition or smooth crossover? | What form of matter exists at the ultra-dense centers of the heaviest neutron stars—ordinary neutrons and protons, exotic hyperons, or deconfined quark matter? | At baryon number densities 2 n_0 <= n_B <= 8 n_0 and zero temperature in beta-equilibrated neutron-star interiors, what is the speed-of-sound profile c_s^2(n_B) = dP/d epsilon, the maximum Tolman-Oppenheimer-Volkoff mass M_TOV, and does a strong first-order deconfinement phase transition produce twin-star mass-radius b... | compact_objects_accretion_high_energy | 8 | Compact Objects, Accretion, and High-Energy Astrophysics | white_dwarfs_and_thermonuclear_transients | [] | mechanism | [
"compact_object",
"star",
"nonthermal_particle"
] | population_level | Astrophysical systems in white dwarfs and thermonuclear transients | [
"km_to_1000km",
"1000km_to_rsun",
"au"
] | [
{
"name": "compact_object_populations",
"redshift_min": 0,
"redshift_max": 1.5,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 9.3
}
] | [
"x_ray",
"radio_cm_m_lowfreq",
"gamma_ray",
"gravitational_wave",
"optical"
] | [
"NICER",
"IXPE",
"XRISM",
"Chandra",
"XMM-Newton"
] | [
"NICER X-ray pulse-profile mass-radius posteriors",
"radio pulsar Shapiro delay masses (PSR J0740+6620)",
"binary neutron star tidal deformability Lambda and post-merger kilohertz GW peak frequency f_2"
] | [
"pressure-energy density relation P(epsilon)",
"sound speed squared c_s^2(n_B)",
"maximum non-rotating neutron star mass M_TOV",
"quark deconfinement threshold density"
] | [
"mass distribution of binary neutron stars in LIGO/Virgo/KAGRA clustering near 1.35 M_sun"
] | [
"NICER hot-spot surface geometry and atmospheric composition modeling",
"nuclear chiral EFT truncation above 1.5 n_0 and perturbative QCD matching below 40 n_0"
] | [
"hadronic equation of state with repulsive three-body forces versus hybrid crossover quark-hadron equation of state (masquerade problem)"
] | open | true | partial_observational_constraint | open_consensus | 2026-10-16T00:00:00 | NICER radius measurements (~12.4 km at 1.4 and 2.08 M_sun) and GW170817 tidal deformability rule out extreme soft and stiff equations of state, but smooth quark-hadron crossovers and stiff nucleonic models yield nearly identical macroscopic M(R) curves ('the masquerade problem'). | multimessenger | decade_scale | Sub-2% radius measurements across 1.2-2.2 M_sun neutron stars with NewAthena/eXTP, together with kilohertz post-merger gravitational-wave spectroscopy in Cosmic Explorer and Einstein Telescope detecting or excluding a phase-transition frequency shift Delta f_2. | Current observations from NICER, IXPE, XRISM constrain pressure-energy density relation P(epsilon), but systematic uncertainties in NICER hot-spot surface geometry and atmospheric composition modeling prevent a definitive resolution. | [
"Baseline astrophysical mechanism in white dwarfs and thermonuclear transients constrained by NICER, IXPE",
"Alternative non-equilibrium, feedback, or multi-component physical model for Cold Dense Matter Equation of State and Existence of Deconfined Quark "
] | [
"High-significance multi-wavelength or dynamical measurement of NICER X-ray pulse-profile mass-radius posteriors using NICER, IXPE, XRISM.",
"Breaking the model degeneracy between hadronic equation of state with repulsive three-body forces versus hybrid crossover quark- to better than 3-5 sigma."
] | Resolving this question in Compact Objects, Accretion, and High-Energy Astrophysics is essential for calibrating pressure-energy density relation P(epsilon) and testing fundamental astrophysical theory. | General relativistic compact objects, supranuclear dense matter equations of state, pulsar magnetospheric electrodynamics, and black hole accretion disk/jet magnetohydrodynamics. | 4 | NICER radius measurements (~12.4 km at 1.4 and 2.08 M_sun) and GW170817 tidal deformability rule out extreme soft and stiff equations of state, but smooth quark-hadron crossovers and stiff nucleonic models yield nearly identical macroscopic M(R) curves ('the masquerade problem'). | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Panel on Compact Objects and Energetic Phenomena, Question COEP-1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-019660",
"citation": "German (2023, Astrophysics & Astronomy Literature)",
... | [
"UAST-000060",
"UAST-000061",
"UAST-000062",
"UAST-000063",
"UAST-000064",
"UAST-000065",
"UAST-001871",
"UAST-001872",
"UAST-001873",
"UAST-001874",
"UAST-001875",
"UAST-001876",
"UAST-001877",
"UAST-001878",
"UAST-001879",
"UAST-021052",
"UAST-020727",
"UAST-022515"
] | null | [] | [
"compact_objects_accretion_high_energy",
"white_dwarfs_and_thermonuclear_transients",
"neutron star interior equation of state",
"deconfined quark cores",
"maximum neutron star mass M_TOV"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000011 | UAST-000011 | uast-000011-emission-mechanism-and-progenitor-diversity-of-repeating-versus-apparently-non-repeat | Emission Mechanism and Progenitor Diversity of Repeating versus Apparently Non-Repeating Fast Radio Bursts | Are all extragalactic fast radio bursts powered by magnetars formed across both core-collapse and delayed merger/accretion-induced collapse channels, and is their coherent gigahertz radio emission generated inside the closed magnetosphere near the neutron star surface or in relativistic magnetized shocks at >>10^{10} c... | Do all fast radio bursts come from highly magnetized neutron stars, and is the radio flash produced close to the star's surface or far out in a shock wave? | Across the extragalactic fast radio burst population, do repeating and apparently one-off FRBs represent distinct progenitor classes or evolutionary stages of magnetar engines, and does the coherent radiation mechanism operate via magnetospheric curvature/maser plasma processes at r ~ 10^6-10^8 cm or synchrotron maser ... | transients_gravitational_waves_multimessenger | 9 | Transients, Gravitational Waves, and Multi-Messenger Astronomy | fast_radio_bursts_and_coherent_radio_transients | [] | origin | [
"transient",
"compact_object",
"galaxy"
] | population_level | Astrophysical systems in fast radio bursts and coherent radio transients | [
"km_to_1000km",
"au",
"pc",
"gpc"
] | [
{
"name": "time_domain_and_multimessenger_universe",
"redshift_min": 0,
"redshift_max": 6,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.8
}
] | [
"gravitational_wave",
"radio_cm_m_lowfreq",
"optical",
"x_ray",
"gamma_ray",
"near_ir"
] | [
"LIGO-Virgo-KAGRA",
"CHIME/FRB",
"DSA-110",
"ASKAP",
"NANOGrav/EPTA/PPTA/IPTA"
] | [
"sub-microsecond burst temporal microstructure",
"polarization position-angle swings and circular polarization fractions",
"host-galaxy stellar population ages and globular-cluster offsets (e.g., FRB 20200120E in M81)"
] | [
"emission radius r_em",
"Lorentz factor and magnetization sigma of the emitting plasma",
"progenitor delay-time distribution"
] | [
"instrumental fluence thresholds and repetition-rate censorship making low-rate repeaters appear one-off"
] | [
"propagation-induced Faraday conversion, scintillation, and plasma lensing in the circumburst medium"
] | [
"intrinsic magnetospheric polarization swings versus propagation effects in a magnetized wind nebula"
] | partially_solved | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | While FRB 200428 from Galactic magnetar SGR 1935+2154 established that magnetars can produce FRBs, the discovery of FRB 20200120E in an old M81 globular cluster requires delayed formation channels, and nanosecond-to-microsecond temporal structures and polarization swings challenge pure far-away shock models while high-... | multimessenger | near_term_1_to_5_years | Sub-arcsecond VLBI localization and polarimetric microstructure analysis of >=1,000 repeaters and non-repeaters with CHIME Outriggers, DSA-2000, and SKAO, plus simultaneous X-ray/optical counterpart detections. | Current observations from LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110 constrain emission radius r_em, but systematic uncertainties in propagation-induced Faraday conversion, scintillation, and plasma lens prevent a definitive resolution. | [
"Baseline astrophysical mechanism in fast radio bursts and coherent radio transients constrained by LIGO-Virgo-KAGRA, CHIME/FRB",
"Alternative non-equilibrium, feedback, or multi-component physical model for Emission Mechanism and Progenitor Diversity of Repeating versus Appare"
] | [
"High-significance multi-wavelength or dynamical measurement of sub-microsecond burst temporal microstructure using LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110.",
"Breaking the model degeneracy between intrinsic magnetospheric polarization swings versus propagation effects in a magnetized wi to better than 3-5 sigma."
] | Resolving this question in Transients, Gravitational Waves, and Multi-Messenger Astronomy is essential for calibrating emission radius r_em and testing fundamental astrophysical theory. | Time-domain astrophysics, gravitational-wave data analysis and source astrophysics, coherent radiative processes in magnetars/FRBs, and relativistic blast-wave hydrodynamics. | 3 | While FRB 200428 from Galactic magnetar SGR 1935+2154 established that magnetars can produce FRBs, the discovery of FRB 20200120E in an old M81 globular cluster requires delayed formation channels, and nanosecond-to-microsecond temporal structures and polarization swings challenge pure far-away shock models while high-... | true | 0 | [
{
"source_id": "SRC-AST-000006",
"support_type": "direct_open_question",
"locator": "SKAO Transient Science Working Group: Fast Radio Bursts, Question FRB-1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-022062",
"citation": "Zhang et al. (2026, arXiv (astro-ph.HE))",
"sup... | [
"UAST-000012",
"UAST-000066",
"UAST-000067",
"UAST-000068",
"UAST-000069",
"UAST-000070",
"UAST-000071",
"UAST-002179",
"UAST-002180",
"UAST-002181",
"UAST-002182",
"UAST-002183",
"UAST-002184",
"UAST-002185",
"UAST-002186",
"UAST-023182",
"UAST-023393",
"UAST-014273"
] | null | [] | [
"transients_gravitational_waves_multimessenger",
"fast_radio_bursts_and_coherent_radio_transients",
"fast radio bursts (FRBs)",
"magnetar coherent emission",
"FRB host-galaxy demographics"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000006). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000012 | UAST-000012 | uast-000012-astrophysical-supermassive-black-hole-binary-versus-cosmological-origin-of-the-nanohe | Astrophysical Supermassive Black Hole Binary versus Cosmological Origin of the Nanohertz Stochastic Gravitational-Wave Background | Is the nanohertz stochastic gravitational-wave background evidenced by pulsar timing arrays (NANOGrav, EPTA/InPTA, PPTA, CPTA) produced entirely by an astrophysical population of inspiraling supermassive black hole binaries, or does it include a cosmological contribution from cosmic strings, phase transitions, or scala... | Does the low-frequency gravitational-wave hum detected by pulsar timing arrays come from pairs of giant black holes orbiting each other across the universe, or from exotic physics in the early universe? | In the 1-100 nHz pulsar timing array band where Hellings-Downs spatial correlations follow h_c(f) = A_yr (f / f_yr)^{alpha} with A_yr ~ 2.4 x 10^{-15}, does the spectral slope alpha, high-frequency discreetness/anisotropy, and resolution of the final-parsec problem confirm supermassive black hole binaries (alpha = -2/3... | transients_gravitational_waves_multimessenger | 9 | Transients, Gravitational Waves, and Multi-Messenger Astronomy | fast_radio_bursts_and_coherent_radio_transients | [] | population_evolution | [
"transient",
"compact_object",
"galaxy"
] | population_level | Astrophysical systems in fast radio bursts and coherent radio transients | [
"km_to_1000km",
"au",
"pc",
"gpc"
] | [
{
"name": "time_domain_and_multimessenger_universe",
"redshift_min": 0,
"redshift_max": 6,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.8
}
] | [
"gravitational_wave",
"radio_cm_m_lowfreq",
"optical",
"x_ray",
"gamma_ray",
"near_ir"
] | [
"LIGO-Virgo-KAGRA",
"CHIME/FRB",
"DSA-110",
"ASKAP",
"NANOGrav/EPTA/PPTA/IPTA"
] | [
"Hellings-Downs angular cross-correlation curve",
"nanohertz GW strain spectrum h_c(f)",
"spatial anisotropy C_ell^{GW} and continuous-wave single-source detections"
] | [
"SMBH binary merger rate and environmental hardening timescale",
"strain spectral index alpha",
"fractional energy density Omega_GW(f)"
] | [
"sky-distribution asymmetry of timed millisecond pulsars"
] | [
"solar-system ephemeris modeling",
"interstellar dispersion measure and pulsar intrinsic red spin noise"
] | [
"gas/stellar-driven eccentric SMBH binary turnover at low frequencies versus cosmological first-order phase transition spectrum"
] | open | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | The 2023 PTA datasets achieved 3-4 sigma evidence for Hellings-Downs correlations with a slightly flatter spectrum than a purely GW-driven circular SMBH binary power law (alpha = -2/3), which is compatible with both environmentally hardened massive SMBH binaries and several early-universe models. | multimessenger | decade_scale | Detection of discrete continuous-wave individual SMBH binaries and frequency-dependent strain anisotropy in IPTA DR3, DSA-2000, and SKAO timing of >=200 millisecond pulsars. | Current observations from LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110 constrain SMBH binary merger rate and environmental hardening timescale, but systematic uncertainties in solar-system ephemeris modeling prevent a definitive resolution. | [
"Baseline astrophysical mechanism in fast radio bursts and coherent radio transients constrained by LIGO-Virgo-KAGRA, CHIME/FRB",
"Alternative non-equilibrium, feedback, or multi-component physical model for Astrophysical Supermassive Black Hole Binary versus Cosmological Origi"
] | [
"High-significance multi-wavelength or dynamical measurement of Hellings-Downs angular cross-correlation curve using LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110.",
"Breaking the model degeneracy between gas/stellar-driven eccentric SMBH binary turnover at low frequencies versus cosmological f to better than 3-5 sigma."
... | Resolving this question in Transients, Gravitational Waves, and Multi-Messenger Astronomy is essential for calibrating SMBH binary merger rate and environmental hardening timescale and testing fundamental astrophysical theory. | Time-domain astrophysics, gravitational-wave data analysis and source astrophysics, coherent radiative processes in magnetars/FRBs, and relativistic blast-wave hydrodynamics. | 4 | The 2023 PTA datasets achieved 3-4 sigma evidence for Hellings-Downs correlations with a slightly flatter spectrum than a purely GW-driven circular SMBH binary power law (alpha = -2/3), which is compatible with both environmentally hardened massive SMBH binaries and several early-universe models. | true | 0 | [
{
"source_id": "SRC-AST-000018",
"support_type": "direct_open_question",
"locator": "Section 4 & 5: Astrophysical and Cosmological Interpretations of the GWB, Question PTA-1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-008216",
"citation": "Gardiner et al. (2026, arXiv (astr... | [
"UAST-000011",
"UAST-010665",
"UAST-008402",
"UAST-004614"
] | null | [] | [
"transients_gravitational_waves_multimessenger",
"fast_radio_bursts_and_coherent_radio_transients",
"nanohertz gravitational-wave background",
"supermassive black hole binaries",
"pulsar timing arrays"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000018). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000013 | UAST-000013 | uast-000013-astrophysical-source-classes-and-acceleration-mechanism-of-ultra-high-energy-cosmic-r | Astrophysical Source Classes and Acceleration Mechanism of Ultra-High-Energy Cosmic Rays Above 10^{18.5} eV | Which extragalactic astrophysical sources—relativistic AGN jets, radio-galaxy lobes, starburst wind termination shocks, gamma-ray bursts, or tidal disruption events—accelerate ultra-high-energy cosmic rays above the ankle (E > 10^{18.5} eV) up to 10^{20} eV, and what accounts for the progressive transition toward heavi... | Which cosmic powerhouses accelerate the highest-energy particles in the universe above ten billion billion electronvolts, and why do those particles become heavier nuclei at the highest energies? | For ultra-high-energy cosmic rays between the ankle at 5 x 10^{18} eV and the flux suppression above 4 x 10^{19} eV, what source population and rigidity-dependent acceleration cutoff E_max(Z) = Z E_{max,p} reproduce the Pierre Auger and Telescope Array energy spectrum, <X_max> and sigma(X_max) mass composition, and int... | cosmic_rays_neutrinos_nonthermal | 10 | Cosmic Rays, Neutrinos, and the Nonthermal Universe | ultra_high_energy_cosmic_rays | [] | mechanism | [
"nonthermal_particle",
"compact_object",
"agn_quasar",
"galaxy"
] | population_level | Astrophysical systems in ultra high energy cosmic rays | [
"au",
"pc",
"kpc",
"mpc"
] | [
{
"name": "nonthermal_and_high_energy_universe",
"redshift_min": 0,
"redshift_max": 4,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.2
}
] | [
"cosmic_ray",
"neutrino",
"gamma_ray",
"x_ray",
"radio_cm_m_lowfreq"
] | [
"Pierre Auger Observatory",
"Telescope Array",
"IceCube",
"KM3NeT",
"LHAASO"
] | [
"extensive air shower depth of maximum X_max and muon number N_mu",
"arrival direction dipole and hotspot correlations",
"cosmogenic EeV neutrino flux"
] | [
"nuclear charge Z and mass number A distribution",
"maximum proton acceleration rigidity R_max",
"extragalactic and Galactic magnetic deflection angles"
] | [
"GZK and photodisintegration attenuation horizon limiting sources above 50 EeV to the local supercluster volume"
] | [
"hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) at center-of-mass energies >100 TeV (the muon puzzle)",
"uncertain Galactic and extragalactic magnetic field models"
] | [
"rigidity-dependent Peters cycle acceleration cutoff at the source versus propagation photodisintegration in the source environment"
] | open | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | Magnetic deflections of intermediate-mass nuclei (CNO to Si/Fe) smear point-source arrival directions across tens of degrees, and hadronic air-shower model uncertainties complicate per-event rigidity reconstruction. | multimessenger | decade_scale | Event-by-event charge/mass discrimination from AugerPrime radio+scintillator upgrades and GCOS, combined with IceCube-Gen2/RNO-G cosmogenic EeV neutrino detections and updated LHCf/forward-collider hadronic models. | Current observations from Pierre Auger Observatory, Telescope Array, IceCube constrain nuclear charge Z and mass number A distribution, but systematic uncertainties in hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) at prevent a definitive resolution. | [
"Baseline astrophysical mechanism in ultra high energy cosmic rays constrained by Pierre Auger Observatory, Telescope Array",
"Alternative non-equilibrium, feedback, or multi-component physical model for Astrophysical Source Classes and Acceleration Mechanism of Ultra-High-"
] | [
"High-significance multi-wavelength or dynamical measurement of extensive air shower depth of maximum X_max and muon number N_mu using Pierre Auger Observatory, Telescope Array, IceCube.",
"Breaking the model degeneracy between rigidity-dependent Peters cycle acceleration cutoff at the source versus propagation p... | Resolving this question in Cosmic Rays, Neutrinos, and the Nonthermal Universe is essential for calibrating nuclear charge Z and mass number A distribution and testing fundamental astrophysical theory. | High-energy particle astrophysics, diffusive shock acceleration and relativistic magnetic reconnection, cosmic-ray propagation and magnetohydrodynamic turbulence, and multimessenger neutrino/gamma-ray radiative transfer. | 4 | Magnetic deflections of intermediate-mass nuclei (CNO to Si/Fe) smear point-source arrival directions across tens of degrees, and hadronic air-shower model uncertainties complicate per-event rigidity reconstruction. | true | 0 | [
{
"source_id": "SRC-AST-000015",
"support_type": "direct_open_question",
"locator": "Ginzburg Problem 26 & Astro2020 Multi-Messenger Frontier, Problem UHECR-1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-024980",
"citation": "The Pierre Auger Collaboration (2023, JCAP05(2023... | [
"UAST-000072",
"UAST-000073",
"UAST-000074",
"UAST-000075",
"UAST-000076",
"UAST-000077",
"UAST-002451",
"UAST-002452",
"UAST-002453",
"UAST-002454",
"UAST-002455",
"UAST-002456",
"UAST-002457",
"UAST-002458",
"UAST-002459",
"UAST-025932",
"UAST-026189",
"UAST-012749"
] | null | [] | [
"cosmic_rays_neutrinos_nonthermal",
"ultra_high_energy_cosmic_rays",
"ultra-high-energy cosmic rays (UHECRs)",
"extragalactic particle accelerators",
"UHECR mass composition and anisotropy"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000015). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000014 | UAST-000014 | uast-000014-physical-origin-of-the-exoplanet-radius-valley-separating-super-earths-and-sub-neptun | Physical Origin of the Exoplanet Radius Valley Separating Super-Earths and Sub-Neptunes | Is the bimodal radius valley at R_p ~ 1.5-2.0 R_Earth separating rocky super-Earths from volatile-rich sub-Neptunes carved primarily by XUV-driven photoevaporation, core-powered atmospheric mass loss, or primordial gas-poor versus water-world formation pathways? | Why are there relatively few exoplanets with sizes between 1.5 and 2.0 times Earth's radius, and is this gap caused by starlight stripping their atmospheres, heat from their own cores, or how they formed? | In the close-in exoplanet population (P < 100 days) around FGKM host stars, how does the dependence of the radius-valley location R_valley(P, M_*, t_age) on orbital period, stellar mass, system age, and planet bulk density rho_p discriminate among XUV photoevaporation, core-powered mass loss, and water-rich migration m... | exoplanets_planetary_system_formation | 11 | Exoplanets and Planetary-System Formation | protoplanetary_disks_and_planet_formation | [] | model_discrimination | [
"exoplanet",
"protoplanetary_disk",
"star"
] | population_level | Astrophysical systems in protoplanetary disks and planet formation | [
"km_to_1000km",
"1000km_to_rsun",
"au"
] | [
{
"name": "protoplanetary_disks_to_mature_systems",
"redshift_min": 0,
"redshift_max": 0.01,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 0.1
}
] | [
"near_ir",
"mid_ir",
"optical",
"mm_submm",
"uv"
] | [
"JWST",
"ALMA",
"TESS",
"Kepler",
"PLATO"
] | [
"radius-period-stellar-mass valley slope d log R_valley / d log P and d log R_valley / d log M_*",
"bulk mass-radius relation M_p(R_p)",
"He I 10830 A and Ly-alpha escaping atmosphere transits",
"JWST transmission spectra of sub-Neptunes"
] | [
"H/He envelope mass fraction f_env",
"water/volatile ice mass fraction",
"atmospheric mass-loss timescale tau_loss"
] | [
"transit geometric probability P_tr ~ a^{-1} and radial-velocity follow-up bias toward bright, quiet stars"
] | [
"host-star radius and age uncertainties",
"high-altitude photochemical hazes muting JWST transmission features"
] | [
"interior composition degeneracy on the mass-radius diagram between a rocky core with a ~1% H2/He envelope and a 50% H2O steam/supercritical water world"
] | open | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | Photoevaporation and core-powered mass loss predict similar slopes in the radius-period plane around FGK stars, while mass-radius measurements alone cannot break the interior degeneracy between H/He-enveloped rocky cores and volatile-rich water worlds without atmospheric mean-molecular-weight determinations. | observational_and_theoretical | near_term_1_to_5_years | Age-resolved occurrence rates from PLATO and Roman across 10 Myr to 10 Gyr stars combined with JWST and Ariel atmospheric mean-molecular-weight and C/O/H2O abundance measurements for >=100 sub-Neptunes. | Current observations from JWST, ALMA, TESS constrain H/He envelope mass fraction f_env, but systematic uncertainties in host-star radius and age uncertainties prevent a definitive resolution. | [
"Baseline astrophysical mechanism in protoplanetary disks and planet formation constrained by JWST, ALMA",
"Alternative non-equilibrium, feedback, or multi-component physical model for Physical Origin of the Exoplanet Radius Valley Separating Super-Earths"
] | [
"High-significance multi-wavelength or dynamical measurement of radius-period-stellar-mass valley slope d log R_valley / d log P and d log R_valley / d lo using JWST, ALMA, TESS.",
"Breaking the model degeneracy between interior composition degeneracy on the mass-radius diagram between a rocky core with a ~1% to ... | Resolving this question in Exoplanets and Planetary-System Formation is essential for calibrating H/He envelope mass fraction f_env and testing fundamental astrophysical theory. | Exoplanet detection and characterization, planetary atmospheric radiative-convective transfer and chemistry, interior structure equations of state, and protoplanetary disk gas-dust hydrodynamics. | 3 | Photoevaporation and core-powered mass loss predict similar slopes in the radius-period plane around FGK stars, while mass-radius measurements alone cannot break the interior degeneracy between H/He-enveloped rocky cores and volatile-rich water worlds without atmospheric mean-molecular-weight determinations. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Worlds and Suns in Context: Pathways to Habitable Worlds, Question WSC-1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-026940",
"citation": "Burn et al. (2024, arXiv (astro-ph.EP))",
"sup... | [
"UAST-000078",
"UAST-000079",
"UAST-000080",
"UAST-000081",
"UAST-000082",
"UAST-000083",
"UAST-002619",
"UAST-002620",
"UAST-002621",
"UAST-002622",
"UAST-002623",
"UAST-002624",
"UAST-002625",
"UAST-002626",
"UAST-002627",
"UAST-027584",
"UAST-027939",
"UAST-027168"
] | null | [] | [
"exoplanets_planetary_system_formation",
"protoplanetary_disks_and_planet_formation",
"exoplanet radius valley (Fulton gap)",
"super-Earths and sub-Neptunes",
"atmospheric escape vs water worlds"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000015 | UAST-000015 | uast-000015-dynamical-existence-versus-collective-gravitational-instability-origin-of-distant-tra | Dynamical Existence versus Collective Gravitational Instability Origin of Distant Trans-Neptunian Orbital Clustering (Planet Nine Hypothesis) | Does the apparent clustering in longitude of perihelion, orbital pole, and argument of perihelion among extreme trans-Neptunian objects (a > 250 AU, q > 30 AU) arise from gravitational shepherding by an undiscovered ~5-10 M_Earth distant planet, from observational survey selection biases, or from self-gravitating disk ... | Are the aligned orbits of the most distant icy objects in the Solar System caused by an undiscovered ninth planet, or are they an artifact of where telescopes have looked? | For extreme trans-Neptunian objects (eTNOs) with semimajor axes a > 250 AU and perihelia q > 40 AU decoupled from strong Neptunian scattering, is the joint distribution of (varpi, Omega, i) statistically incompatible with uniform random angles after accounting for survey pointing history, depth, and cadence, and does a... | solar_system_worlds_small_bodies | 12 | Solar-System Worlds and Small Bodies | giant_planets_and_ice_giants | [] | model_discrimination | [
"solar_system_body",
"dust_and_ice"
] | population_level | Astrophysical systems in giant planets and ice giants | [
"sub_km",
"km_to_1000km",
"au"
] | [
{
"name": "solar_nebula_to_present_solar_system",
"redshift_min": 0,
"redshift_max": 0,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 4.567
}
] | [
"optical",
"near_ir",
"mid_ir",
"mm_submm",
"radio_cm_m_lowfreq",
"uv"
] | [
"Juno",
"Europa Clipper",
"JUICE",
"Dragonfly",
"OSIRIS-REx"
] | [
"orbital elements (a, q, e, i, Omega, varpi) of eTNOs",
"direct wide-field optical/IR and CMB-survey moving-object detections"
] | [
"intrinsic eTNO orbital angle distribution",
"mass M_9 and semimajor axis a_9 of a hypothetical distant planet"
] | [
"severe longitudinal, seasonal, and Galactic-plane pointing biases in heterogeneous TNO discovery surveys"
] | [
"small sample size (N < 30 decoupled eTNOs) and sensitivity to semi-major axis and perihelion cutoff choices"
] | [
"observational pointing bias + Neptunian mean-motion/secular diffusion versus gravitational shepherding by an unseen planet"
] | open | true | partial_observational_constraint | open_consensus | 2026-10-16T00:00:00 | Analyses of heterogeneous discovery catalogs find clustering significance ~3 sigma, whereas uniformly characterized surveys (OSSOS, DES, Bernardinelli et al.) have yielded mixed consistency with a uniform intrinsic distribution due to limited sample sizes. | observational_and_theoretical | near_term_1_to_5_years | Vera C. Rubin Observatory LSST discovering >10x more decoupled eTNOs with a single, fully characterized selection function and either directly detecting a distant planet down to V ~ 24.5 or proving uniform eTNO orbital longitudes. | Current observations from Juno, Europa Clipper, JUICE constrain intrinsic eTNO orbital angle distribution, but systematic uncertainties in small sample size (N < 30 decoupled eTNOs) and sensitivity to semi-maj prevent a definitive resolution. | [
"Baseline astrophysical mechanism in giant planets and ice giants constrained by Juno, Europa Clipper",
"Alternative non-equilibrium, feedback, or multi-component physical model for Dynamical Existence versus Collective Gravitational Instability Origin"
] | [
"High-significance multi-wavelength or dynamical measurement of orbital elements (a, q, e, i, Omega, varpi) of eTNOs using Juno, Europa Clipper, JUICE.",
"Breaking the model degeneracy between observational pointing bias + Neptunian mean-motion/secular diffusion versus gravitational to better than 3-5 sigma."
] | Resolving this question in Solar-System Worlds and Small Bodies is essential for calibrating intrinsic eTNO orbital angle distribution and testing fundamental astrophysical theory. | Planetary geophysics and interior structure, cosmochemistry and meteoritics, orbital dynamics and celestial mechanics, and icy moon oceanography. | 3 | Analyses of heterogeneous discovery catalogs find clustering significance ~3 sigma, whereas uniformly characterized surveys (OSSOS, DES, Bernardinelli et al.) have yielded mixed consistency with a uniform intrinsic distribution due to limited sample sizes. | true | 0 | [
{
"source_id": "SRC-AST-000004",
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},
{
"source_id": "SRC-AST-029752",
"citation": "Porter et al. (2024, arXiv (astro-ph.EP))",
"sup... | [
"UAST-000084",
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"UAST-002933",
"UAST-002934",
"UAST-002935",
"UAST-030193",
"UAST-030203",
"UAST-030859"
] | null | [] | [
"solar_system_worlds_small_bodies",
"giant_planets_and_ice_giants",
"extreme trans-Neptunian objects (eTNOs)",
"distant Solar System architecture",
"Planet Nine hypothesis"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000004). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000016 | UAST-000016 | uast-000016-abiotic-photochemical-false-positives-versus-biological-production-of-oxygen-methane | Abiotic Photochemical False Positives versus Biological Production of Oxygen, Methane, and Organosulfur Gases in Temperate Exoplanet Atmospheres | Under what host-star ultraviolet spectral energy distributions and planetary redox conditions can simultaneous detections of atmospheric O2/O3 with CH4/CO2 or trace organosulfur gases (such as dimethyl sulfide) on temperate terrestrial or Hycean exoplanets be uniquely distinguished from abiotic photochemical and outgas... | When telescopes detect gases like oxygen, methane, or dimethyl sulfide in an exoplanet's atmosphere, what additional clues are needed to prove they come from life rather than non-biological chemistry? | In transmission, emission, and reflected-light spectroscopy of temperate terrestrial and sub-Neptune/Hycean exoplanets around M and FGK dwarfs, what combination of disequilibrium gas abundances (O2, O3, CH4, CO2, CO, N2O, H2O, DMS), isotopic ratios, and surface-atmosphere redox indicators rules out abiotic H2O/CO2 phot... | astrobiology_habitability_biosignatures_technosignatures | 13 | Astrobiology, Habitability, Biosignatures, and Technosignatures | technosignatures_and_seti | [] | detection_or_characterization | [
"exoplanet",
"solar_system_body",
"interstellar_medium",
"star"
] | population_level | Astrophysical systems in technosignatures and seti | [
"km_to_1000km",
"au",
"pc"
] | [
{
"name": "prebiotic_to_planetary_biospheres",
"redshift_min": 0,
"redshift_max": 0.05,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 4.5
}
] | [
"near_ir",
"mid_ir",
"uv",
"optical",
"radio_cm_m_lowfreq"
] | [
"JWST",
"Habitable Worlds Observatory",
"ELT",
"LIFE",
"Europa Clipper"
] | [
"JWST, ELT, and HWO transmission/reflected-light molecular absorption bands",
"O2-O2 1.27 micron collision-induced absorption",
"CO and H2O abundance ratios",
"host-star FUV/NUV Ly-alpha flux"
] | [
"surface biotic vs abiotic gas fluxes",
"planetary mantle/crustal redox state",
"ocean vs magma-ocean or supercritical-envelope lower boundary"
] | [
"transit spectroscopy feasibility strongly favoring M-dwarf hosts with extreme pre-main-sequence XUV irradiation histories"
] | [
"incomplete high-temperature/high-pressure cross-section line lists for trace organosulfur and hydrocarbon gases",
"stellar photospheric heterogeneity (Transit Light Source Effect) and correlated instrumental noise"
] | [
"overlapping 3.3-3.5 micron absorption bands of CH4, DMS, CS2, and C2H6 in low-SNR JWST transmission spectra; abiotic serpentinization + CO2 reduction versus methanogenesis"
] | open | true | partial_observational_constraint | open_consensus | 2026-10-16T00:00:00 | Single-gas detections and low-SNR multi-gas claims (such as tentative DMS hints in K2-18 b alongside CH4 and CO2) are degenerate with overlapping hydrocarbon/sulfur cross sections and abiotic interior-atmosphere chemistry in H2-rich sub-Neptunes. | observational_and_theoretical | decade_scale | High-SNR multi-band JWST + ELT high-resolution cross-correlation spectroscopy and Habitable Worlds Observatory UV-optical-NIR reflected-light spectra jointly measuring O2, O3, CH4, CO2, H2O, and excluding abiotic false-positive markers (CO, O4). | Current observations from JWST, Habitable Worlds Observatory, ELT constrain surface biotic vs abiotic gas fluxes, but systematic uncertainties in incomplete high-temperature/high-pressure cross-section line lists for prevent a definitive resolution. | [
"Baseline astrophysical mechanism in technosignatures and seti constrained by JWST, Habitable Worlds Observatory",
"Alternative non-equilibrium, feedback, or multi-component physical model for Abiotic Photochemical False Positives versus Biological Production of "
] | [
"High-significance multi-wavelength or dynamical measurement of JWST, ELT, and HWO transmission/reflected-light molecular absorption bands using JWST, Habitable Worlds Observatory, ELT.",
"Breaking the model degeneracy between overlapping 3.3-3.5 micron absorption bands of CH4, DMS, CS2, and C2H6 in low-SNR JWST ... | Resolving this question in Astrobiology, Habitability, Biosignatures, and Technosignatures is essential for calibrating surface biotic vs abiotic gas fluxes and testing fundamental astrophysical theory. | Astrobiology, planetary climate and atmospheric photochemistry, prebiotic organic chemistry and volatile delivery, biosignature false-positive assessment, and technosignature search methodology. | 4 | Single-gas detections and low-SNR multi-gas claims (such as tentative DMS hints in K2-18 b alongside CH4 and CO2) are degenerate with overlapping hydrocarbon/sulfur cross sections and abiotic interior-atmosphere chemistry in H2-rich sub-Neptunes. | true | 0 | [
{
"source_id": "SRC-AST-000017",
"support_type": "direct_open_question",
"locator": "NFoLD Biosignatures Standards of Evidence Framework (Levels 1-5), Standard B-1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-031754",
"citation": "Mitchell et al. (2025, arXiv (astro-ph.EP))"... | [
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"UAST-003136",
"UAST-003137",
"UAST-003138",
"UAST-032028",
"UAST-027163",
"UAST-031884"
] | null | [] | [
"astrobiology_habitability_biosignatures_technosignatures",
"technosignatures_and_seti",
"exoplanet atmospheric biosignatures",
"abiotic oxygen and methane false positives",
"Hycean and terrestrial worlds (e.g., K2-18 b, TRAPPIST-1 e)"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000017). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000017 | UAST-000017 | uast-000017-quantitative-partition-between-alfv-nic-wave-turbulence-and-impulsive-nanoflare-recon | Quantitative Partition Between Alfvénic Wave Turbulence and Impulsive Nanoflare Reconnection in Heating the Solar Corona and Accelerating the Solar Wind | What are the relative quantitative energy fluxes contributed by low-frequency Alfvénic wave turbulence cascades versus impulsive magnetic reconnection ('nanoflares' and interchange reconnection jets/switchbacks) to heating the quiet and active solar corona above 10^6 K and accelerating the fast and slow solar wind? | How much of the Sun's million-degree corona heating and solar wind acceleration comes from magnetic waves versus tiny magnetic reconnection explosions? | From the solar chromosphere/transition region (1.01 R_sun) through the Alfvén critical surface (10-20 R_sun) probed by Parker Solar Probe and Solar Orbiter, what fraction of the coronal radiative/conductive loss budget (10^5-10^7 erg cm^{-2} s^{-1}) is supplied by ion-cyclotron/stochastic Alfvén-wave dissipation versus... | solar_stellar_activity_heliospheric | 14 | Solar, Stellar-Activity, and Heliospheric Astronomy | solar_interior_dynamo_and_cycle | [] | model_discrimination | [
"star",
"heliosphere",
"solar_system_body"
] | population_level | Astrophysical systems in solar interior dynamo and cycle | [
"sub_km",
"km_to_1000km",
"1000km_to_rsun",
"au"
] | [
{
"name": "modern_solar_and_stellar_cycles",
"redshift_min": 0,
"redshift_max": 0.001,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 0.01
}
] | [
"uv",
"x_ray",
"optical",
"radio_cm_m_lowfreq",
"cosmic_ray"
] | [
"Parker Solar Probe",
"Solar Orbiter",
"DKIST",
"SDO",
"IRIS"
] | [
"EUV/X-ray Differential Emission Measure DEM(T) and nonthermal line broadening",
"Parker Solar Probe in-situ Poynting flux, proton/alpha temperature anisotropy, and switchback statistics",
"DKIST high-resolution chromospheric magnetograms"
] | [
"volumetric coronal heating rate Q(r)",
"nanoflare energy distribution slope alpha_E",
"turbulent cascade dissipation rate epsilon_turb"
] | [
"line-of-sight optically thin integration across multistranded coronal loops obscuring individual sub-resolution reconnection events"
] | [
"non-equilibrium ionization lags during impulsive heating",
"single-spacecraft spatiotemporal ambiguity when mapping in-situ solar wind streams back to coronal footpoints"
] | [
"secondary Alfvén waves generated by interchange reconnection jets versus photospherically driven wave turbulence"
] | open | true | conflicting_measurements | active_debate | 2026-10-16T00:00:00 | Parker Solar Probe and Solar Orbiter have revealed ubiquitous interchange-reconnection jets ('picoflare jets') and magnetic switchbacks near the Alfvén surface while EUV spectroscopy shows high-temperature emission components in active regions, proving both mechanisms operate without yet closing the global energy budge... | observational_and_theoretical | decade_scale | Coordinated multi-point observations linking DKIST/MUSE sub-arcsecond coronal spectroscopy with Parker Solar Probe and Solar Orbiter perihelion in-situ plasma/field measurements across the Alfvén critical zone. | Current observations from Parker Solar Probe, Solar Orbiter, DKIST constrain volumetric coronal heating rate Q(r), but systematic uncertainties in non-equilibrium ionization lags during impulsive heating prevent a definitive resolution. | [
"Baseline astrophysical mechanism in solar interior dynamo and cycle constrained by Parker Solar Probe, Solar Orbiter",
"Alternative non-equilibrium, feedback, or multi-component physical model for Quantitative Partition Between Alfvénic Wave Turbulence and Impulsive "
] | [
"High-significance multi-wavelength or dynamical measurement of EUV/X-ray Differential Emission Measure DEM(T) and nonthermal line broadening using Parker Solar Probe, Solar Orbiter, DKIST.",
"Breaking the model degeneracy between secondary Alfvén waves generated by interchange reconnection jets versus photospher... | Resolving this question in Solar, Stellar-Activity, and Heliospheric Astronomy is essential for calibrating volumetric coronal heating rate Q(r) and testing fundamental astrophysical theory. | Solar and stellar magnetohydrodynamics, helioseismology and dynamo theory, magnetic reconnection and kinetic plasma turbulence, and heliospheric space physics. | 4 | Parker Solar Probe and Solar Orbiter have revealed ubiquitous interchange-reconnection jets ('picoflare jets') and magnetic switchbacks near the Alfvén surface while EUV spectroscopy shows high-temperature emission components in active regions, proving both mechanisms operate without yet closing the global energy budge... | true | 0 | [
{
"source_id": "SRC-AST-000005",
"support_type": "direct_open_question",
"locator": "Heliophysics Decadal Survey Guiding Question 1: Coronal Heating and Solar Wind Acceleration, Question H-1",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-033283",
"citation": "B et al. (2026, A... | [
"UAST-000096",
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] | null | [] | [
"solar_stellar_activity_heliospheric",
"solar_interior_dynamo_and_cycle",
"solar coronal heating problem",
"solar wind acceleration",
"magnetic switchbacks and nanoflares"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000005). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000018 | UAST-000018 | uast-000018-primordial-local-non-gaussianity-amplitude-f-nl-local-from-multi-tracer-galaxy-survey | Primordial Local Non-Gaussianity Amplitude f_NL^local from Multi-Tracer Galaxy Surveys | Does the primordial curvature perturbation exhibit local-type non-Gaussianity with |f_NL^local| >= 1 detectable through scale-dependent halo bias in wide-field spectroscopic and photometric galaxy surveys, or were primordial fluctuations generated by single-field slow-roll inflation with f_NL^local ~ O(n_s - 1) << 1? | Does the primordial curvature perturbation exhibit local-type non-Gaussianity with |f_NL^local| >= 1 detectable through scale-dependent halo bias in wide-field spectroscopic and photometric galaxy surveys, or were primordial fluctuations generated by single-field slow-roll inflation with f_NL^local ~ O(n_s - 1) << 1? | Does the primordial curvature perturbation exhibit local-type non-Gaussianity with |f_NL^local| >= 1 detectable through scale-dependent halo bias in wide-field spectroscopic and photometric galaxy surveys, or were primordial fluctuations generated by single-field slow-roll inflation with f_NL^local ~ O(n_s - 1) << 1? H... | cosmology_early_universe | 1 | Cosmology and the Early Universe | inflation_and_primordial_initial_conditions | [] | value_or_bound | [
"large_scale_structure",
"cosmic_background"
] | population_level | Astrophysical systems in inflation and primordial initial conditions | [
"cosmological_horizon",
"gpc"
] | [
{
"name": "inflation_and_recombination",
"redshift_min": 1100,
"redshift_max": null,
"lookback_time_gyr_min": 13.78,
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}
] | [
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"cmb_mm_submm"
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"Simons Observatory",
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"CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB",
"Baryon acoustic oscillation distance ratios D_M(z)/r_d and D_H(z)/r_d",
"Redshifted 21 cm brightness temperature fluctuations delta T_b(k, z)"
] | [
"Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL)",
"Comoving sound horizon r_d and Hubble expansion rate H(z)",
"Neutral hydrogen fraction x_HI(z) and ionizing photon escape fraction f_esc"
] | [
"Cosmic variance at low multipoles l < 30",
"Lyman-alpha line-of-sight damping-wing absorption bias at z > 7"
] | [
"Galactic polarized thermal dust and synchrotron foreground subtraction residuals",
"Cepheid/TRGB photometric crowding and metallicity zero-point calibration"
] | [
"Sound horizon r_d vs late-time dark energy equation of state w(z)",
"Optical depth tau_reio vs primordial scalar amplitude A_s"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Cosmology and the Early Universe community syntheses as of 2026-10-16. | survey_statistical | decade_scale | Discriminating Baseline astrophysical mechanism in inflation and primordial initial condit from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB. | Current observations from Planck, JWST, DESI constrain Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL), but systematic uncertainties in Galactic polarized thermal dust and synchrotron foreground subtraction prevent a definitive resolution. | [
"Baseline astrophysical mechanism in inflation and primordial initial conditions constrained by Planck, JWST",
"Alternative non-equilibrium, feedback, or multi-component physical model for Primordial Local Non-Gaussianity Amplitude f_NL^local from Multi-Trace"
] | [
"High-significance multi-wavelength or dynamical measurement of CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB using Planck, JWST, DESI.",
"Breaking the model degeneracy between Sound horizon r_d vs late-time dark energy equation of state w(z) to better than 3-5 sigma."
] | Resolving this question in Cosmology and the Early Universe is essential for calibrating Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL) and testing fundamental astrophysical theory. | Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Appendix B, Priority Area: New Messengers and New Physics, p. B-14",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-001314",
"citation": "Stahl et al. (2024, arXiv (astro-ph.CO))",
"support_... | [
"UAST-000001",
"UAST-004509",
"UAST-008368",
"UAST-003993"
] | null | [] | [
"cosmology_early_universe",
"inflation_and_primordial_initial_conditions",
"non_gaussianity",
"f_NL",
"scale_dependent_bias",
"inflation"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000019 | UAST-000019 | uast-000019-primordial-cmb-mu-and-y-type-blackbody-spectral-distortions-from-silk-damping | Primordial CMB mu- and y-Type Blackbody Spectral Distortions from Silk Damping | What is the exact amplitude of the primordial chemical-potential (mu-type) and Compton (y-type) spectral distortions of the cosmic microwave background generated by acoustic Silk damping at small scales (50 <= k <= 10^4 Mpc^-1), and do pre-recombination energy injection processes exceed the standard adiabatic LambdaCDM... | What is the exact amplitude of the primordial chemical-potential (mu-type) and Compton (y-type) spectral distortions of the cosmic microwave background generated by acoustic Silk damping at small scales (50 <= k <= 10^4 Mpc^-1), and do pre-recombination energy injection processes exceed the standard adiabatic LambdaCDM... | What is the exact amplitude of the primordial chemical-potential (mu-type) and Compton (y-type) spectral distortions of the cosmic microwave background generated by acoustic Silk damping at small scales (50 <= k <= 10^4 Mpc^-1), and do pre-recombination energy injection processes exceed the standard adiabatic LambdaCDM... | cosmology_early_universe | 1 | Cosmology and the Early Universe | cmb_anisotropies_polarization_and_spectral_distortions | [] | value_or_bound | [
"cosmic_background",
"early_universe"
] | population_level | Astrophysical systems in cmb anisotropies polarization and spectral distortions | [
"cosmological_horizon",
"mpc"
] | [
{
"name": "inflation_and_recombination",
"redshift_min": 1100,
"redshift_max": null,
"lookback_time_gyr_min": 13.78,
"lookback_time_gyr_max": 13.8
}
] | [
"cmb_mm_submm",
"far_ir"
] | [
"Planck",
"JWST",
"DESI",
"Simons Observatory",
"CMB-S4"
] | [
"CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB",
"Baryon acoustic oscillation distance ratios D_M(z)/r_d and D_H(z)/r_d",
"Redshifted 21 cm brightness temperature fluctuations delta T_b(k, z)"
] | [
"Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL)",
"Comoving sound horizon r_d and Hubble expansion rate H(z)",
"Neutral hydrogen fraction x_HI(z) and ionizing photon escape fraction f_esc"
] | [
"Cosmic variance at low multipoles l < 30",
"Lyman-alpha line-of-sight damping-wing absorption bias at z > 7"
] | [
"Galactic polarized thermal dust and synchrotron foreground subtraction residuals",
"Cepheid/TRGB photometric crowding and metallicity zero-point calibration"
] | [
"Sound horizon r_d vs late-time dark energy equation of state w(z)",
"Optical depth tau_reio vs primordial scalar amplitude A_s"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Cosmology and the Early Universe community syntheses as of 2026-10-16. | survey_statistical | decade_scale | Discriminating Baseline astrophysical mechanism in cmb anisotropies polarization and spect from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB. | Current observations from Planck, JWST, DESI constrain Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL), but systematic uncertainties in Galactic polarized thermal dust and synchrotron foreground subtraction prevent a definitive resolution. | [
"Baseline astrophysical mechanism in cmb anisotropies polarization and spectral distortions constrained by Planck, JWST",
"Alternative non-equilibrium, feedback, or multi-component physical model for Primordial CMB mu- and y-Type Blackbody Spectral Distortions from Silk"
] | [
"High-significance multi-wavelength or dynamical measurement of CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB using Planck, JWST, DESI.",
"Breaking the model degeneracy between Sound horizon r_d vs late-time dark energy equation of state w(z) to better than 3-5 sigma."
] | Resolving this question in Cosmology and the Early Universe is essential for calibrating Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL) and testing fundamental astrophysical theory. | Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000002",
"support_type": "direct_open_question",
"locator": "Section 3.1: Voyage 2050 White Paper on CMB Spectral Distortions, p. 18",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-002471",
"citation": "Farhang et al. (2012, Astronomy Journal)",
"sup... | [
"UAST-000001",
"UAST-005666",
"UAST-005075",
"UAST-000176"
] | null | [] | [
"cosmology_early_universe",
"cmb_anisotropies_polarization_and_spectral_distortions",
"spectral_distortions",
"mu_distortion",
"Silk_damping",
"CMB"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000002). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000020 | UAST-000020 | uast-000020-cosmological-neutrino-mass-sum-from-combined-cmb-lensing-and-bao-clustering | Cosmological Neutrino Mass Sum from Combined CMB Lensing and BAO Clustering | What is the sum of the three active neutrino mass eigenstates Sigma m_nu inferred from late-time suppression of matter clustering and gravitational lensing of the CMB, and why do current BAO + CMB lensing combinations favor upper bounds near or slightly below the minimal normal-hierarchy threshold of 0.059 eV? | What is the sum of the three active neutrino mass eigenstates Sigma m_nu inferred from late-time suppression of matter clustering and gravitational lensing of the CMB, and why do current BAO + CMB lensing combinations favor upper bounds near or slightly below the minimal normal-hierarchy threshold of 0.059 eV? | What is the sum of the three active neutrino mass eigenstates Sigma m_nu inferred from late-time suppression of matter clustering and gravitational lensing of the CMB, and why do current BAO + CMB lensing combinations favor upper bounds near or slightly below the minimal normal-hierarchy threshold of 0.059 eV? Highligh... | cosmology_early_universe | 1 | Cosmology and the Early Universe | baryogenesis_nucleosynthesis_and_recombination | [] | tension_resolution | [
"cosmic_background",
"large_scale_structure"
] | population_level | Astrophysical systems in baryogenesis nucleosynthesis and recombination | [
"cosmological_horizon",
"gpc"
] | [
{
"name": "inflation_and_recombination",
"redshift_min": 1100,
"redshift_max": null,
"lookback_time_gyr_min": 13.78,
"lookback_time_gyr_max": 13.8
}
] | [
"cmb_mm_submm",
"optical",
"near_ir"
] | [
"Planck",
"JWST",
"DESI",
"Simons Observatory",
"CMB-S4"
] | [
"CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB",
"Baryon acoustic oscillation distance ratios D_M(z)/r_d and D_H(z)/r_d",
"Redshifted 21 cm brightness temperature fluctuations delta T_b(k, z)"
] | [
"Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL)",
"Comoving sound horizon r_d and Hubble expansion rate H(z)",
"Neutral hydrogen fraction x_HI(z) and ionizing photon escape fraction f_esc"
] | [
"Cosmic variance at low multipoles l < 30",
"Lyman-alpha line-of-sight damping-wing absorption bias at z > 7"
] | [
"Galactic polarized thermal dust and synchrotron foreground subtraction residuals",
"Cepheid/TRGB photometric crowding and metallicity zero-point calibration"
] | [
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UAST-000025 | UAST-000025 | uast-000025-velocity-dependent-self-interacting-dark-matter-cross-section-sigma-m-across-dwarf-ga | Velocity-Dependent Self-Interacting Dark Matter Cross Section Sigma/m Across Dwarf Galaxies to Galaxy Clusters | Can a velocity-dependent self-interacting dark matter cross section sigma/m(v) simultaneously explain the diversity of inner rotation curve slopes in dwarf irregular and low-surface-brightness galaxies (sigma/m ~ 1-5 cm^2 g^-1 at v ~ 30-100 km s^-1) while satisfying the upper bound sigma/m < 0.1-0.3 cm^2 g^-1 in mergin... | Can a velocity-dependent self-interacting dark matter cross section sigma/m(v) simultaneously explain the diversity of inner rotation curve slopes in dwarf irregular and low-surface-brightness galaxies (sigma/m ~ 1-5 cm^2 g^-1 at v ~ 30-100 km s^-1) while satisfying the upper bound sigma/m < 0.1-0.3 cm^2 g^-1 in mergin... | Can a velocity-dependent self-interacting dark matter cross section sigma/m(v) simultaneously explain the diversity of inner rotation curve slopes in dwarf irregular and low-surface-brightness galaxies (sigma/m ~ 1-5 cm^2 g^-1 at v ~ 30-100 km s^-1) while satisfying the upper bound sigma/m < 0.1-0.3 cm^2 g^-1 in mergin... | dark_matter_dark_energy_fundamental_cosmology | 2 | Dark Matter, Dark Energy, and Fundamental Cosmology | dark_matter_astrophysical_signatures | [] | model_discrimination | [
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UAST-000026 | UAST-000026 | uast-000026-redshift-space-distortion-growth-rate-f-sigma-8-z-vs-general-relativity-predictions | Redshift-Space Distortion Growth Rate f*sigma_8(z) vs General Relativity Predictions | Does the linear structure growth rate parameter f(z)*sigma_8(z) measured from anisotropic galaxy clustering and peculiar velocity surveys at 0.1 <= z <= 2.0 follow the General Relativistic prediction gamma = d ln f / d ln Omega_m(z) ~ 0.55, or is late-time cosmic growth suppressed relative to the background expansion h... | Does the linear structure growth rate parameter f(z)*sigma_8(z) measured from anisotropic galaxy clustering and peculiar velocity surveys at 0.1 <= z <= 2.0 follow the General Relativistic prediction gamma = d ln f / d ln Omega_m(z) ~ 0.55, or is late-time cosmic growth suppressed relative to the background expansion h... | Does the linear structure growth rate parameter f(z)*sigma_8(z) measured from anisotropic galaxy clustering and peculiar velocity surveys at 0.1 <= z <= 2.0 follow the General Relativistic prediction gamma = d ln f / d ln Omega_m(z) ~ 0.55, or is late-time cosmic growth suppressed relative to the background expansion h... | dark_matter_dark_energy_fundamental_cosmology | 2 | Dark Matter, Dark Energy, and Fundamental Cosmology | dark_energy_and_cosmic_acceleration | [] | value_or_bound | [
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000003). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000027 | UAST-000027 | uast-000027-gravitational-slip-parameter-eta-phi-psi-on-linear-cosmological-scales | Gravitational Slip Parameter eta = Phi/Psi on Linear Cosmological Scales | Is the cosmological gravitational slip parameter eta(k, z) = Phi/Psi relating the Newtonian potential Psi (governing non-relativistic peculiar motions) to the spatial curvature potential Phi (governing weak gravitational lensing) equal to unity across 0.01 <= k <= 1 h Mpc^-1 and 0 <= z <= 2, as required by General Rela... | Is the cosmological gravitational slip parameter eta(k, z) = Phi/Psi relating the Newtonian potential Psi (governing non-relativistic peculiar motions) to the spatial curvature potential Phi (governing weak gravitational lensing) equal to unity across 0.01 <= k <= 1 h Mpc^-1 and 0 <= z <= 2, as required by General Rela... | Is the cosmological gravitational slip parameter eta(k, z) = Phi/Psi relating the Newtonian potential Psi (governing non-relativistic peculiar motions) to the spatial curvature potential Phi (governing weak gravitational lensing) equal to unity across 0.01 <= k <= 1 h Mpc^-1 and 0 <= z <= 2, as required by General Rela... | dark_matter_dark_energy_fundamental_cosmology | 2 | Dark Matter, Dark Energy, and Fundamental Cosmology | modified_gravity_and_gravitational_tests | [] | value_or_bound | [
"large_scale_structure",
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] | population_level | Astrophysical systems in modified gravity and gravitational tests | [
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{
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"citation": "Sinde et al. (2026, arXiv (astro-ph.CO))",
"support_type": "expli... | [
"UAST-000003",
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] | null | [] | [
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"modified_gravity_and_gravitational_tests",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000002). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000028 | UAST-000028 | uast-000028-primordial-black-hole-dark-matter-fraction-in-the-asteroid-to-sublunar-mass-window | Primordial Black Hole Dark Matter Fraction in the Asteroid-to-Sublunar Mass Window | What observational signatures—such as femtolensing/diffraction of fast radio bursts and gamma-ray bursts, white dwarf or neutron star capture, or microlensing of stars in M31—can definitively bound or detect primordial black holes in the currently open mass window 10^-16 M_sun <= M_PBH <= 10^-10 M_sun where they could ... | What observational signatures—such as femtolensing/diffraction of fast radio bursts and gamma-ray bursts, white dwarf or neutron star capture, or microlensing of stars in M31—can definitively bound or detect primordial black holes in the currently open mass window 10^-16 M_sun <= M_PBH <= 10^-10 M_sun where they could ... | What observational signatures—such as femtolensing/diffraction of fast radio bursts and gamma-ray bursts, white dwarf or neutron star capture, or microlensing of stars in M31—can definitively bound or detect primordial black holes in the currently open mass window 10^-16 M_sun <= M_PBH <= 10^-10 M_sun where they could ... | dark_matter_dark_energy_fundamental_cosmology | 2 | Dark Matter, Dark Energy, and Fundamental Cosmology | primordial_black_holes_and_exotic_relics | [] | value_or_bound | [
"dark_sector",
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] | population_level | Astrophysical systems in primordial black holes and exotic relics | [
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"support_type": ... | [
"UAST-000003",
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"primordial_black_holes_and_exotic_relics",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000003). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000029 | UAST-000029 | uast-000029-axion-like-particle-photon-conversion-signatures-in-magnetized-galaxy-clusters-and-ne | Axion-Like Particle Photon Conversion Signatures in Magnetized Galaxy Clusters and Neutron Star Magnetospheres | Do ultralight axion-like particles (ALPs) produce detectable spectral oscillations in X-ray/gamma-ray AGN spectra transmitted through magnetized intracluster media or narrow radio conversion lines in pulsar magnetospheres across the coupling range g_agamma ~ 10^-13 to 10^-11 GeV^-1? | Do ultralight axion-like particles (ALPs) produce detectable spectral oscillations in X-ray/gamma-ray AGN spectra transmitted through magnetized intracluster media or narrow radio conversion lines in pulsar magnetospheres across the coupling range g_agamma ~ 10^-13 to 10^-11 GeV^-1? | Do ultralight axion-like particles (ALPs) produce detectable spectral oscillations in X-ray/gamma-ray AGN spectra transmitted through magnetized intracluster media or narrow radio conversion lines in pulsar magnetospheres across the coupling range g_agamma ~ 10^-13 to 10^-11 GeV^-1? Highlighted as a key community resea... | dark_matter_dark_energy_fundamental_cosmology | 2 | Dark Matter, Dark Energy, and Fundamental Cosmology | dark_matter_astrophysical_signatures | [] | value_or_bound | [
"dark_sector",
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] | population_level | Astrophysical systems in dark matter astrophysical signatures | [
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"source_id": "SRC-AST-023403",
"citation": "Sigl (2017, Phys. Rev. D 96, 103014 (2017))",
... | [
"UAST-000003",
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"dark_matter_dark_energy_fundamental_cosmology",
"dark_matter_astrophysical_signatures",
"axions",
"ALPs",
"intracluster_magnetic_field",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000004). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000030 | UAST-000030 | uast-000030-cosmic-void-density-profiles-and-peculiar-velocity-outflows-as-probes-of-dark-energy | Cosmic Void Density Profiles and Peculiar Velocity Outflows as Probes of Dark Energy and Neutrino Mass | Can dynamic Alcock-Paczynski distortions and peculiar velocity outflow profiles around cosmic voids (R_v ~ 10-50 h^-1 Mpc) be modeled free of galaxy bias systematics to break degeneracies between massive neutrino free-streaming and dynamical dark energy? | Can dynamic Alcock-Paczynski distortions and peculiar velocity outflow profiles around cosmic voids (R_v ~ 10-50 h^-1 Mpc) be modeled free of galaxy bias systematics to break degeneracies between massive neutrino free-streaming and dynamical dark energy? | Can dynamic Alcock-Paczynski distortions and peculiar velocity outflow profiles around cosmic voids (R_v ~ 10-50 h^-1 Mpc) be modeled free of galaxy bias systematics to break degeneracies between massive neutrino free-streaming and dynamical dark energy? Highlighted as a key community research question in Voyage 2050: ... | large_scale_structure_igm_cosmic_web | 3 | Large-Scale Structure, Intergalactic Medium, and Cosmic Web | cosmic_web_filaments_sheets_and_voids | [] | model_discrimination | [
"large_scale_structure",
"dark_sector"
] | population_level | Astrophysical systems in cosmic web filaments sheets and voids | [
"10_to_100_mpc",
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"Extragalactic Faraday rotation measure grids RM and fast radio burst dispersion measures... | [
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{
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000003). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000031 | UAST-000031 | uast-000031-thermal-history-and-he-ii-reionization-heating-of-the-intergalactic-medium-at-z-2-5 | Thermal History and He II Reionization Heating of the Intergalactic Medium at z = 2-5 | How do the temperature-density relation T = T_0 (Delta)^(gamma - 1) and pressure smoothing scale lambda_P of the intergalactic medium evolve across 2 <= z <= 5 in high-resolution Lyman-alpha forest spectra, and what is the exact spatial patchiness and timing of He II reionization driven by quasars? | How do the temperature-density relation T = T_0 (Delta)^(gamma - 1) and pressure smoothing scale lambda_P of the intergalactic medium evolve across 2 <= z <= 5 in high-resolution Lyman-alpha forest spectra, and what is the exact spatial patchiness and timing of He II reionization driven by quasars? | How do the temperature-density relation T = T_0 (Delta)^(gamma - 1) and pressure smoothing scale lambda_P of the intergalactic medium evolve across 2 <= z <= 5 in high-resolution Lyman-alpha forest spectra, and what is the exact spatial patchiness and timing of He II reionization driven by quasars? Highlighted as a key... | large_scale_structure_igm_cosmic_web | 3 | Large-Scale Structure, Intergalactic Medium, and Cosmic Web | intergalactic_medium_and_lya_forest | [] | population_evolution | [
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"intergalactic_medium_and_lya_forest",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000032 | UAST-000032 | uast-000032-multiphase-mass-and-metal-budget-of-the-circumgalactic-medium-around-l-and-dwarf-gala | Multiphase Mass and Metal Budget of the Circumgalactic Medium Around L* and Dwarf Galaxies | What fractions of a galaxy's cosmic baryon and metal budgets reside in the cool (T ~ 10^4 K), intermediate warm-hot (T ~ 10^5-10^6 K, O VI / Ne VIII), and hot virialized (T > 10^6 K) phases of the circumgalactic medium out to 1-2 virial radii, and how do inflow and outflow recycling timescales depend on halo mass? | What fractions of a galaxy's cosmic baryon and metal budgets reside in the cool (T ~ 10^4 K), intermediate warm-hot (T ~ 10^5-10^6 K, O VI / Ne VIII), and hot virialized (T > 10^6 K) phases of the circumgalactic medium out to 1-2 virial radii, and how do inflow and outflow recycling timescales depend on halo mass? | What fractions of a galaxy's cosmic baryon and metal budgets reside in the cool (T ~ 10^4 K), intermediate warm-hot (T ~ 10^5-10^6 K, O VI / Ne VIII), and hot virialized (T > 10^6 K) phases of the circumgalactic medium out to 1-2 virial radii, and how do inflow and outflow recycling timescales depend on halo mass? High... | large_scale_structure_igm_cosmic_web | 3 | Large-Scale Structure, Intergalactic Medium, and Cosmic Web | circumgalactic_medium_and_baryon_cycle | [] | mechanism | [
"circumgalactic_medium",
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{
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{
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"citation": "Lan et al. (2018, Monthly notices of the Royal Astronom... | [
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] | null | [] | [
"large_scale_structure_igm_cosmic_web",
"circumgalactic_medium_and_baryon_cycle",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000033 | UAST-000033 | uast-000033-hydrostatic-mass-bias-and-non-thermal-pressure-support-in-galaxy-clusters | Hydrostatic Mass Bias and Non-Thermal Pressure Support in Galaxy Clusters | What fraction of total pressure support in galaxy clusters from the core out to R_500 and R_200 arises from bulk turbulence, cosmic rays, and magnetic fields (the hydrostatic mass bias 1 - b), and how does this bias vary with cluster mass, dynamical state, and redshift in X-ray and Sunyaev-Zel'dovich cluster cosmology? | What fraction of total pressure support in galaxy clusters from the core out to R_500 and R_200 arises from bulk turbulence, cosmic rays, and magnetic fields (the hydrostatic mass bias 1 - b), and how does this bias vary with cluster mass, dynamical state, and redshift in X-ray and Sunyaev-Zel'dovich cluster cosmology? | What fraction of total pressure support in galaxy clusters from the core out to R_500 and R_200 arises from bulk turbulence, cosmic rays, and magnetic fields (the hydrostatic mass bias 1 - b), and how does this bias vary with cluster mass, dynamical state, and redshift in X-ray and Sunyaev-Zel'dovich cluster cosmology?... | large_scale_structure_igm_cosmic_web | 3 | Large-Scale Structure, Intergalactic Medium, and Cosmic Web | galaxy_clusters_intracluster_medium_and_sz | [] | value_or_bound | [
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] | population_level | Astrophysical systems in galaxy clusters intracluster medium and sz | [
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{
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{
"source_id": "SRC-AST-006624",
"citation": "Hurier et al. (2018, Astronomy & Astrophysics)",
"supp... | [
"UAST-000005",
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] | null | [] | [
"large_scale_structure_igm_cosmic_web",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000005). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000034 | UAST-000034 | uast-000034-strength-and-origin-of-intergalactic-magnetic-fields-in-cosmic-filaments-and-voids | Strength and Origin of Intergalactic Magnetic Fields in Cosmic Filaments and Voids | Were intergalactic magnetic fields in cosmic filaments (B ~ 10-100 nG) and voids (B >= 10^-16 G inferred from TeV blazar gamma-ray cascades) seeded by primordial magnetogenesis in the early universe or by astrophysical magnetized outflows and Biermann batteries during structure formation? | Were intergalactic magnetic fields in cosmic filaments (B ~ 10-100 nG) and voids (B >= 10^-16 G inferred from TeV blazar gamma-ray cascades) seeded by primordial magnetogenesis in the early universe or by astrophysical magnetized outflows and Biermann batteries during structure formation? | Were intergalactic magnetic fields in cosmic filaments (B ~ 10-100 nG) and voids (B >= 10^-16 G inferred from TeV blazar gamma-ray cascades) seeded by primordial magnetogenesis in the early universe or by astrophysical magnetized outflows and Biermann batteries during structure formation? Highlighted as a key community... | large_scale_structure_igm_cosmic_web | 3 | Large-Scale Structure, Intergalactic Medium, and Cosmic Web | cosmic_magnetic_fields_and_large_scale_fields | [] | origin | [
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{
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{
"source_id": "SRC-AST-006581",
"citation": "Kobayashi et al. (2019, Phys. Rev. D 100, 023524 (2019))",
"support_t... | [
"UAST-000005",
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"large_scale_structure_igm_cosmic_web",
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"Faraday_rotation",
"primordial_magnetogenesis",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000004). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000035 | UAST-000035 | uast-000035-particle-re-acceleration-efficiency-in-mega-parsec-cluster-radio-halos-and-relics | Particle Re-Acceleration Efficiency in Mega-Parsec Cluster Radio Halos and Relics | How do low-Mach-number intracluster merger shocks (M ~ 1.5-3) and magnetohydrodynamic turbulence accelerate relativistic electrons across megaparsec scales in diffuse cluster radio relics and halos when standard diffusive shock acceleration from the thermal pool is inefficient? | How do low-Mach-number intracluster merger shocks (M ~ 1.5-3) and magnetohydrodynamic turbulence accelerate relativistic electrons across megaparsec scales in diffuse cluster radio relics and halos when standard diffusive shock acceleration from the thermal pool is inefficient? | How do low-Mach-number intracluster merger shocks (M ~ 1.5-3) and magnetohydrodynamic turbulence accelerate relativistic electrons across megaparsec scales in diffuse cluster radio relics and halos when standard diffusive shock acceleration from the thermal pool is inefficient? Highlighted as a key community research q... | large_scale_structure_igm_cosmic_web | 3 | Large-Scale Structure, Intergalactic Medium, and Cosmic Web | galaxy_clusters_intracluster_medium_and_sz | [] | mechanism | [
"galaxy_cluster",
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] | population_level | Astrophysical systems in galaxy clusters intracluster medium and sz | [
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{
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"Extragalactic Faraday rotation measure grids RM and fast radio burst dispersion measures... | [
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UAST-000036 | UAST-000036 | uast-000036-origin-of-nitrogen-overabundant-and-carbon-enhanced-ism-in-z-8-galaxies | Origin of Nitrogen-Overabundant and Carbon-Enhanced ISM in z > 8 Galaxies | Why do luminous high-redshift galaxies at z ~ 8-11 (such as GN-z11 and GHZ2) exhibit extreme nitrogen-to-oxygen abundance ratios (log(N/O) > -0.5, far above normal metal-poor dwarf galaxies), and does this chemical signature arise from Wolf-Rayet winds, supermassive stars in proto-globular clusters, tidal disruption ev... | Why do luminous high-redshift galaxies at z ~ 8-11 (such as GN-z11 and GHZ2) exhibit extreme nitrogen-to-oxygen abundance ratios (log(N/O) > -0.5, far above normal metal-poor dwarf galaxies), and does this chemical signature arise from Wolf-Rayet winds, supermassive stars in proto-globular clusters, tidal disruption ev... | Why do luminous high-redshift galaxies at z ~ 8-11 (such as GN-z11 and GHZ2) exhibit extreme nitrogen-to-oxygen abundance ratios (log(N/O) > -0.5, far above normal metal-poor dwarf galaxies), and does this chemical signature arise from Wolf-Rayet winds, supermassive stars in proto-globular clusters, tidal disruption ev... | galaxies_supermassive_black_holes | 4 | Galaxies and Supermassive Black Holes | high_redshift_galaxy_formation_and_first_galaxies | [] | origin | [
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UAST-000037 | UAST-000037 | uast-000037-origin-and-intrinsic-scatter-of-the-radial-acceleration-relation-and-baryonic-tully-f | Origin and Intrinsic Scatter of the Radial Acceleration Relation and Baryonic Tully-Fisher Relation | Can dissipative galaxy formation and stellar/AGN feedback within cold dark matter halos fully account for the tight normalization, low intrinsic scatter (< 0.1 dex), and characteristic acceleration scale a_0 ~ 1.2 x 10^-10 m s^-2 of the baryonic Tully-Fisher and radial acceleration relations across five decades in stel... | Can dissipative galaxy formation and stellar/AGN feedback within cold dark matter halos fully account for the tight normalization, low intrinsic scatter (< 0.1 dex), and characteristic acceleration scale a_0 ~ 1.2 x 10^-10 m s^-2 of the baryonic Tully-Fisher and radial acceleration relations across five decades in stel... | Can dissipative galaxy formation and stellar/AGN feedback within cold dark matter halos fully account for the tight normalization, low intrinsic scatter (< 0.1 dex), and characteristic acceleration scale a_0 ~ 1.2 x 10^-10 m s^-2 of the baryonic Tully-Fisher and radial acceleration relations across five decades in stel... | galaxies_supermassive_black_holes | 4 | Galaxies and Supermassive Black Holes | galaxy_dynamics_scaling_relations_and_morphology | [] | model_discrimination | [
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UAST-000038 | UAST-000038 | uast-000038-nature-and-black-hole-to-stellar-mass-ratio-of-jwst-little-red-dots-at-z-4-9 | Nature and Black Hole-to-Stellar Mass Ratio of JWST 'Little Red Dots' at z = 4-9 | Are the compact, red optical-continuum, broad-Balmer-line sources ('Little Red Dots') discovered by JWST at 4 <= z <= 9 heavily dust-reddened super-Eddington accreting black holes with overmassive M_BH/M_* ~ 0.01-0.1 ratios, or compact starburst cores with dense gas envelopes mimicking broad AGN emission and lacking br... | Are the compact, red optical-continuum, broad-Balmer-line sources ('Little Red Dots') discovered by JWST at 4 <= z <= 9 heavily dust-reddened super-Eddington accreting black holes with overmassive M_BH/M_* ~ 0.01-0.1 ratios, or compact starburst cores with dense gas envelopes mimicking broad AGN emission and lacking br... | Are the compact, red optical-continuum, broad-Balmer-line sources ('Little Red Dots') discovered by JWST at 4 <= z <= 9 heavily dust-reddened super-Eddington accreting black holes with overmassive M_BH/M_* ~ 0.01-0.1 ratios, or compact starburst cores with dense gas envelopes mimicking broad AGN emission and lacking br... | galaxies_supermassive_black_holes | 4 | Galaxies and Supermassive Black Holes | supermassive_black_hole_seeds_and_growth | [] | object_nature | [
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UAST-000039 | UAST-000039 | uast-000039-momentum-boost-and-multiphase-coupling-of-ultrafast-outflows-to-kpc-scale-molecular-a | Momentum Boost and Multiphase Coupling of Ultrafast Outflows to kpc-Scale Molecular AGN Winds | Do nuclear relativistic X-ray ultrafast outflows (v ~ 0.1-0.3c) drive kiloparsec-scale cold molecular and ionized galactic winds via energy-conserving adiabatic expansion (yielding momentum boosts p_dot / (L/c) ~ 5-20) or momentum-conserving radiative shocks, and how efficiently do they deplete cold star-forming gas in... | Do nuclear relativistic X-ray ultrafast outflows (v ~ 0.1-0.3c) drive kiloparsec-scale cold molecular and ionized galactic winds via energy-conserving adiabatic expansion (yielding momentum boosts p_dot / (L/c) ~ 5-20) or momentum-conserving radiative shocks, and how efficiently do they deplete cold star-forming gas in... | Do nuclear relativistic X-ray ultrafast outflows (v ~ 0.1-0.3c) drive kiloparsec-scale cold molecular and ionized galactic winds via energy-conserving adiabatic expansion (yielding momentum boosts p_dot / (L/c) ~ 5-20) or momentum-conserving radiative shocks, and how efficiently do they deplete cold star-forming gas in... | galaxies_supermassive_black_holes | 4 | Galaxies and Supermassive Black Holes | agn_physics_winds_and_jets | [] | mechanism | [
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{
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UAST-000040 | UAST-000040 | uast-000040-final-parsec-hardening-timescale-and-coalescence-efficiency-of-supermassive-black-hol | Final-Parsec Hardening Timescale and Coalescence Efficiency of Supermassive Black Hole Binaries | After a galaxy merger brings two supermassive black holes (10^6-10^10 M_sun) to parsec separations, what combination of triaxial stellar loss-cone replenishment, circumbinary gas disk torques, and triple-SMBH interactions drives the binary across the sub-parsec regime into the gravitational-wave-dominated inspiral band... | After a galaxy merger brings two supermassive black holes (10^6-10^10 M_sun) to parsec separations, what combination of triaxial stellar loss-cone replenishment, circumbinary gas disk torques, and triple-SMBH interactions drives the binary across the sub-parsec regime into the gravitational-wave-dominated inspiral band... | After a galaxy merger brings two supermassive black holes (10^6-10^10 M_sun) to parsec separations, what combination of triaxial stellar loss-cone replenishment, circumbinary gas disk torques, and triple-SMBH interactions drives the binary across the sub-parsec regime into the gravitational-wave-dominated inspiral band... | galaxies_supermassive_black_holes | 4 | Galaxies and Supermassive Black Holes | galaxy_mergers_and_environmental_processing | [] | mechanism | [
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"Dust obscuration bias in rest-frame UV selections of massive galaxies"
] | [
"Broad-line region virial factor f_BLR geometric uncertainty and single-epoch M_BH calibration",
"Stellar initial mass function and dust attenuation law assumptions in SED fitting"
] | [
"Dust-reddened AGN continuum vs compact starburst emission in high-z Little Red Dots",
"Preventive halo heating vs ejective gas removal in galaxy quenching"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Galaxies and Supermassive Black Holes community syntheses as of 2026-10-16. | multimessenger | decade_scale | Discriminating Baseline astrophysical mechanism in galaxy mergers and environmental proces from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Rest-frame UV/optical nebular emission line ratios ([O III], H-beta, N III], C I. | Current observations from JWST, ALMA, Chandra constrain Supermassive black hole mass M_BH, Eddington ratio lambda_Edd, and seed formation cha, but systematic uncertainties in Broad-line region virial factor f_BLR geometric uncertainty and single prevent a definitive resolution. | [
"Baseline astrophysical mechanism in galaxy mergers and environmental processing constrained by JWST, ALMA",
"Alternative non-equilibrium, feedback, or multi-component physical model for Final-Parsec Hardening Timescale and Coalescence Efficiency of Superma"
] | [
"High-significance multi-wavelength or dynamical measurement of Rest-frame UV/optical nebular emission line ratios ([O III], H-beta, N III], C IV) and bro using JWST, ALMA, Chandra.",
"Breaking the model degeneracy between Dust-reddened AGN continuum vs compact starburst emission in high-z Little Red Dots to bett... | Resolving this question in Galaxies and Supermassive Black Holes is essential for calibrating Supermassive black hole mass M_BH, Eddington ratio lambda_Edd, and seed formatio and testing fundamental astrophysical theory. | Galaxy formation and evolution, active galactic nucleus accretion and feedback physics, stellar population synthesis, and galactic dynamics. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000006",
"support_type": "direct_open_question",
"locator": "Section 3.2: Massive Black Hole Binaries and the Final Parsec Problem, p. 38",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-022164",
"citation": "Arutkeerthi et al. (2026, arXiv (gr-qc))",
... | [
"UAST-000006",
"UAST-023284",
"UAST-011176",
"UAST-010310"
] | null | [] | [
"galaxies_supermassive_black_holes",
"galaxy_mergers_and_environmental_processing",
"final_parsec_problem",
"SMBH_binaries",
"loss_cone",
"LISA",
"PTA"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000006). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000041 | UAST-000041 | uast-000041-inside-out-vs-morphological-quenching-mechanisms-in-massive-passive-galaxies-at-z-2-5 | Inside-Out vs Morphological Quenching Mechanisms in Massive Passive Galaxies at z = 2-5 | Why do massive galaxies (M_* > 10^10.5 M_sun) already exhibit quiescent, quenched stellar populations by z ~ 3-5, and what is the relative role of preventive halo heating by radio/kinetic AGN feedback versus ejective cold-gas removal or morphological stabilization against disk fragmentation? | Why do massive galaxies (M_* > 10^10.5 M_sun) already exhibit quiescent, quenched stellar populations by z ~ 3-5, and what is the relative role of preventive halo heating by radio/kinetic AGN feedback versus ejective cold-gas removal or morphological stabilization against disk fragmentation? | Why do massive galaxies (M_* > 10^10.5 M_sun) already exhibit quiescent, quenched stellar populations by z ~ 3-5, and what is the relative role of preventive halo heating by radio/kinetic AGN feedback versus ejective cold-gas removal or morphological stabilization against disk fragmentation? Highlighted as a key commun... | galaxies_supermassive_black_holes | 4 | Galaxies and Supermassive Black Holes | quenching_star_formation_and_baryonic_feedback | [] | mechanism | [
"galaxy",
"agn_quasar"
] | population_level | Astrophysical systems in quenching star formation and baryonic feedback | [
"kpc"
] | [
{
"name": "first_galaxies_through_cosmic_noon",
"redshift_min": 0,
"redshift_max": 14,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 13.5
}
] | [
"near_ir",
"mid_ir",
"mm_submm"
] | [
"JWST",
"ALMA",
"Chandra",
"VLT/MUSE",
"SDSS/BOSS"
] | [
"Rest-frame UV/optical nebular emission line ratios ([O III], H-beta, N III], C IV) and broad Balmer line widths",
"Submillimeter CO/C+ molecular kinematics and far-IR dust continuum spectral energy distributions",
"X-ray Fe K-alpha reflection spectra, ultrafast outflow absorption troughs, and VLBI jet proper m... | [
"Supermassive black hole mass M_BH, Eddington ratio lambda_Edd, and seed formation channel",
"Stellar mass M_*, star formation rate SFR, gas depletion timescale, and outflow mass-loading factor eta",
"Dark matter fraction f_DM(r) and baryonic feedback coupling efficiency"
] | [
"Flux-limited Eddington bias favoring luminous quasars and UV-bright starbursts at z > 7",
"Dust obscuration bias in rest-frame UV selections of massive galaxies"
] | [
"Broad-line region virial factor f_BLR geometric uncertainty and single-epoch M_BH calibration",
"Stellar initial mass function and dust attenuation law assumptions in SED fitting"
] | [
"Dust-reddened AGN continuum vs compact starburst emission in high-z Little Red Dots",
"Preventive halo heating vs ejective gas removal in galaxy quenching"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Galaxies and Supermassive Black Holes community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in quenching star formation and baryonic f from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Rest-frame UV/optical nebular emission line ratios ([O III], H-beta, N III], C I. | Current observations from JWST, ALMA, Chandra constrain Supermassive black hole mass M_BH, Eddington ratio lambda_Edd, and seed formation cha, but systematic uncertainties in Broad-line region virial factor f_BLR geometric uncertainty and single prevent a definitive resolution. | [
"Baseline astrophysical mechanism in quenching star formation and baryonic feedback constrained by JWST, ALMA",
"Alternative non-equilibrium, feedback, or multi-component physical model for Inside-Out vs Morphological Quenching Mechanisms in Massive Passive Ga"
] | [
"High-significance multi-wavelength or dynamical measurement of Rest-frame UV/optical nebular emission line ratios ([O III], H-beta, N III], C IV) and bro using JWST, ALMA, Chandra.",
"Breaking the model degeneracy between Dust-reddened AGN continuum vs compact starburst emission in high-z Little Red Dots to bett... | Resolving this question in Galaxies and Supermassive Black Holes is essential for calibrating Supermassive black hole mass M_BH, Eddington ratio lambda_Edd, and seed formatio and testing fundamental astrophysical theory. | Galaxy formation and evolution, active galactic nucleus accretion and feedback physics, stellar population synthesis, and galactic dynamics. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Section 2.2: Unveiling the Hidden Drivers of Galaxy Growth, p. 2-20",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-009494",
"citation": "Bezanson et al. (2019, arXiv (astro-ph.GA))",
"supp... | [
"UAST-000006",
"UAST-011943",
"UAST-010580",
"UAST-010626"
] | null | [] | [
"galaxies_supermassive_black_holes",
"quenching_star_formation_and_baryonic_feedback",
"massive_quiescent_galaxies",
"high_z_quenching",
"AGN_feedback",
"JWST_ALMA"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000042 | UAST-000042 | uast-000042-pattern-speed-slowdown-history-and-dark-halo-dynamical-friction-of-the-galactic-bar | Pattern Speed, Slowdown History, and Dark Halo Dynamical Friction of the Galactic Bar | What is the dynamical friction torque exerted by the Milky Way's dark matter halo on the Galactic bar (current pattern speed Omega_b ~ 35-41 km s^-1 kpc^-1), and do kinematic resonances in the Gaia phase-space spirals and Hercules stream indicate rapid secular bar slowdown or bar-spiral mode coupling? | What is the dynamical friction torque exerted by the Milky Way's dark matter halo on the Galactic bar (current pattern speed Omega_b ~ 35-41 km s^-1 kpc^-1), and do kinematic resonances in the Gaia phase-space spirals and Hercules stream indicate rapid secular bar slowdown or bar-spiral mode coupling? | What is the dynamical friction torque exerted by the Milky Way's dark matter halo on the Galactic bar (current pattern speed Omega_b ~ 35-41 km s^-1 kpc^-1), and do kinematic resonances in the Gaia phase-space spirals and Hercules stream indicate rapid secular bar slowdown or bar-spiral mode coupling? Highlighted as a ... | milky_way_local_group_near_field | 5 | Milky Way, Local Group, and Near-Field Cosmology | milky_way_structure_kinematics_and_potential | [] | mechanism | [
"milky_way_component",
"dark_sector",
"star"
] | population_level | Astrophysical systems in milky way structure kinematics and potential | [
"kpc"
] | [
{
"name": "milky_way_assembly_history",
"redshift_min": 0,
"redshift_max": 4,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.2
}
] | [
"optical",
"near_ir"
] | [
"Gaia",
"SDSS-V",
"APOGEE",
"GALAH",
"WEAVE"
] | [
"Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial velocity) from Gaia",
"High-resolution stellar photospheric elemental abundances ([Fe/H], [alpha/Fe], r- and s-process ratios)",
"Cold stellar stream track density profiles, velocity dispersions, and off-stream spurs"
] | [
"Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial mass M_200",
"Accretion history of disrupted progenitor dwarfs (Gaia-Sausage-Enceladus, Sagittarius, Kraken)",
"Inner dark matter density slope d ln rho / d ln r in Local Group dwarf spheroidals"
] | [
"Three-dimensional interstellar dust extinction in the Galactic plane and inner bulge",
"Binary star orbital motion inflating apparent velocity dispersions in ultra-faint dwarfs"
] | [
"Non-LTE and 3D convective photospheric abundance corrections across giant and dwarf stars",
"Gaia parallax zero-point spatial variations and crowding in globular cluster cores"
] | [
"Orbital velocity anisotropy beta(r) vs inner dark matter cusp/core density profile",
"Secular radial migration vs merger-induced heating in the Galactic disk"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Milky Way, Local Group, and Near-Field Cosmology community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in milky way structure kinematics and pote from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial. | Current observations from Gaia, SDSS-V, APOGEE constrain Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial , but systematic uncertainties in Non-LTE and 3D convective photospheric abundance corrections across gi prevent a definitive resolution. | [
"Baseline astrophysical mechanism in milky way structure kinematics and potential constrained by Gaia, SDSS-V",
"Alternative non-equilibrium, feedback, or multi-component physical model for Pattern Speed, Slowdown History, and Dark Halo Dynamical Friction of t"
] | [
"High-significance multi-wavelength or dynamical measurement of Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial velocity) using Gaia, SDSS-V, APOGEE.",
"Breaking the model degeneracy between Orbital velocity anisotropy beta(r) vs inner dark matter cusp/core density profile to bett... | Resolving this question in Milky Way, Local Group, and Near-Field Cosmology is essential for calibrating Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total vi and testing fundamental astrophysical theory. | Galactic dynamics, action-angle phase-space modeling, stellar nucleosynthesis and chemical evolution, and Local Group near-field cosmology. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000003",
"support_type": "direct_open_question",
"locator": "Section 3.1: Galactic Dynamics with Gaia and Spectroscopic Surveys, p. 45",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-011957",
"citation": "Monari et al. (2016, arXiv (astro-ph.GA))",
"... | [
"UAST-000007",
"UAST-014203",
"UAST-013540",
"UAST-013863"
] | null | [] | [
"milky_way_local_group_near_field",
"milky_way_structure_kinematics_and_potential",
"Galactic_bar",
"pattern_speed",
"dynamical_friction",
"Gaia_phase_spiral"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000003). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000043 | UAST-000043 | uast-000043-origin-of-the-milky-way-alpha-abundance-bimodality-alpha-fe-vs-fe-h-high-and-low-alph | Origin of the Milky Way Alpha-Abundance Bimodality ([alpha/Fe] vs [Fe/H] High- and Low-Alpha Disks) | Was the bimodal distribution of high-[alpha/Fe] (thick disk) and low-[alpha/Fe] (thin disk) stars in the Milky Way produced by a major gas-rich merger (such as Gaia-Sausage-Enceladus at z ~ 2) followed by metal-poor gas accretion, or by secular radial migration and clumpy star formation without requiring a discrete mer... | Was the bimodal distribution of high-[alpha/Fe] (thick disk) and low-[alpha/Fe] (thin disk) stars in the Milky Way produced by a major gas-rich merger (such as Gaia-Sausage-Enceladus at z ~ 2) followed by metal-poor gas accretion, or by secular radial migration and clumpy star formation without requiring a discrete mer... | Was the bimodal distribution of high-[alpha/Fe] (thick disk) and low-[alpha/Fe] (thin disk) stars in the Milky Way produced by a major gas-rich merger (such as Gaia-Sausage-Enceladus at z ~ 2) followed by metal-poor gas accretion, or by secular radial migration and clumpy star formation without requiring a discrete mer... | milky_way_local_group_near_field | 5 | Milky Way, Local Group, and Near-Field Cosmology | galactic_archaeology_and_chemical_evolution | [] | origin | [
"milky_way_component",
"stellar_population"
] | population_level | Astrophysical systems in galactic archaeology and chemical evolution | [
"kpc"
] | [
{
"name": "milky_way_assembly_history",
"redshift_min": 0,
"redshift_max": 4,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.2
}
] | [
"optical",
"near_ir"
] | [
"Gaia",
"SDSS-V",
"APOGEE",
"GALAH",
"WEAVE"
] | [
"Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial velocity) from Gaia",
"High-resolution stellar photospheric elemental abundances ([Fe/H], [alpha/Fe], r- and s-process ratios)",
"Cold stellar stream track density profiles, velocity dispersions, and off-stream spurs"
] | [
"Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial mass M_200",
"Accretion history of disrupted progenitor dwarfs (Gaia-Sausage-Enceladus, Sagittarius, Kraken)",
"Inner dark matter density slope d ln rho / d ln r in Local Group dwarf spheroidals"
] | [
"Three-dimensional interstellar dust extinction in the Galactic plane and inner bulge",
"Binary star orbital motion inflating apparent velocity dispersions in ultra-faint dwarfs"
] | [
"Non-LTE and 3D convective photospheric abundance corrections across giant and dwarf stars",
"Gaia parallax zero-point spatial variations and crowding in globular cluster cores"
] | [
"Orbital velocity anisotropy beta(r) vs inner dark matter cusp/core density profile",
"Secular radial migration vs merger-induced heating in the Galactic disk"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Milky Way, Local Group, and Near-Field Cosmology community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in galactic archaeology and chemical evolu from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial. | Current observations from Gaia, SDSS-V, APOGEE constrain Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial , but systematic uncertainties in Non-LTE and 3D convective photospheric abundance corrections across gi prevent a definitive resolution. | [
"Baseline astrophysical mechanism in galactic archaeology and chemical evolution constrained by Gaia, SDSS-V",
"Alternative non-equilibrium, feedback, or multi-component physical model for Origin of the Milky Way Alpha-Abundance Bimodality ([alpha/Fe] vs [Fe/"
] | [
"High-significance multi-wavelength or dynamical measurement of Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial velocity) using Gaia, SDSS-V, APOGEE.",
"Breaking the model degeneracy between Orbital velocity anisotropy beta(r) vs inner dark matter cusp/core density profile to bett... | Resolving this question in Milky Way, Local Group, and Near-Field Cosmology is essential for calibrating Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total vi and testing fundamental astrophysical theory. | Galactic dynamics, action-angle phase-space modeling, stellar nucleosynthesis and chemical evolution, and Local Group near-field cosmology. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Appendix C: Galactic Archaeology, p. C-19",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-011062",
"citation": "Malhan (2025, The Astrophysical Journal Letters)",
"support_type": "explicit_... | [
"UAST-000007",
"UAST-013308",
"UAST-001230",
"UAST-014566"
] | null | [] | [
"milky_way_local_group_near_field",
"galactic_archaeology_and_chemical_evolution",
"alpha_bimodality",
"thick_disk",
"Gaia_Sausage_Enceladus",
"radial_migration"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000044 | UAST-000044 | uast-000044-plane-of-satellites-phase-space-coherence-around-the-milky-way-m31-and-centaurus-a | Plane of Satellites Phase-Space Coherence Around the Milky Way, M31, and Centaurus A | Is the thin, kinematically coherent plane of satellite galaxies observed around the Milky Way, M31, and Centaurus A a transient alignment enhanced by group infall along cosmic web filaments (including the Magellanic Cloud system) within LambdaCDM, or does it represent a persistent dynamical discrepancy? | Is the thin, kinematically coherent plane of satellite galaxies observed around the Milky Way, M31, and Centaurus A a transient alignment enhanced by group infall along cosmic web filaments (including the Magellanic Cloud system) within LambdaCDM, or does it represent a persistent dynamical discrepancy? | Is the thin, kinematically coherent plane of satellite galaxies observed around the Milky Way, M31, and Centaurus A a transient alignment enhanced by group infall along cosmic web filaments (including the Magellanic Cloud system) within LambdaCDM, or does it represent a persistent dynamical discrepancy? Highlighted as ... | milky_way_local_group_near_field | 5 | Milky Way, Local Group, and Near-Field Cosmology | local_group_dwarfs_and_near_field_cosmology | [] | tension_resolution | [
"galaxy",
"milky_way_component",
"dark_sector"
] | population_level | Astrophysical systems in local group dwarfs and near field cosmology | [
"kpc",
"mpc"
] | [
{
"name": "milky_way_assembly_history",
"redshift_min": 0,
"redshift_max": 4,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.2
}
] | [
"optical",
"near_ir"
] | [
"Gaia",
"SDSS-V",
"APOGEE",
"GALAH",
"WEAVE"
] | [
"Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial velocity) from Gaia",
"High-resolution stellar photospheric elemental abundances ([Fe/H], [alpha/Fe], r- and s-process ratios)",
"Cold stellar stream track density profiles, velocity dispersions, and off-stream spurs"
] | [
"Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial mass M_200",
"Accretion history of disrupted progenitor dwarfs (Gaia-Sausage-Enceladus, Sagittarius, Kraken)",
"Inner dark matter density slope d ln rho / d ln r in Local Group dwarf spheroidals"
] | [
"Three-dimensional interstellar dust extinction in the Galactic plane and inner bulge",
"Binary star orbital motion inflating apparent velocity dispersions in ultra-faint dwarfs"
] | [
"Non-LTE and 3D convective photospheric abundance corrections across giant and dwarf stars",
"Gaia parallax zero-point spatial variations and crowding in globular cluster cores"
] | [
"Orbital velocity anisotropy beta(r) vs inner dark matter cusp/core density profile",
"Secular radial migration vs merger-induced heating in the Galactic disk"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Milky Way, Local Group, and Near-Field Cosmology community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in local group dwarfs and near field cosmo from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial. | Current observations from Gaia, SDSS-V, APOGEE constrain Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial , but systematic uncertainties in Non-LTE and 3D convective photospheric abundance corrections across gi prevent a definitive resolution. | [
"Baseline astrophysical mechanism in local group dwarfs and near field cosmology constrained by Gaia, SDSS-V",
"Alternative non-equilibrium, feedback, or multi-component physical model for Plane of Satellites Phase-Space Coherence Around the Milky Way, M31, a"
] | [
"High-significance multi-wavelength or dynamical measurement of Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial velocity) using Gaia, SDSS-V, APOGEE.",
"Breaking the model degeneracy between Orbital velocity anisotropy beta(r) vs inner dark matter cusp/core density profile to bett... | Resolving this question in Milky Way, Local Group, and Near-Field Cosmology is essential for calibrating Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total vi and testing fundamental astrophysical theory. | Galactic dynamics, action-angle phase-space modeling, stellar nucleosynthesis and chemical evolution, and Local Group near-field cosmology. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000003",
"support_type": "direct_open_question",
"locator": "Section 2.2: Near-Field Cosmology and Satellite Systems, p. 27",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-009697",
"citation": "Oliver et al. (2017, Astron.Astrophys.)",
"support_type"... | [
"UAST-000007",
"UAST-012146",
"UAST-013261",
"UAST-013502"
] | null | [] | [
"milky_way_local_group_near_field",
"local_group_dwarfs_and_near_field_cosmology",
"plane_of_satellites",
"Local_Group",
"proper_motions",
"near_field_cosmology"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000003). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000045 | UAST-000045 | uast-000045-origin-of-density-spurs-and-gaps-in-the-gd-1-and-palomar-5-cold-stellar-streams | Origin of Density Spurs and Gaps in the GD-1 and Palomar 5 Cold Stellar Streams | Were the off-stream spur, density gap, and cocoon structures observed in the thin globular cluster stream GD-1 (and Palomar 5) produced by the gravitational impulse of a dark, starless dark matter subhalo of mass 10^6-10^8 M_sun, or by interactions with giant molecular clouds, the Galactic bar, or spiral arms? | Were the off-stream spur, density gap, and cocoon structures observed in the thin globular cluster stream GD-1 (and Palomar 5) produced by the gravitational impulse of a dark, starless dark matter subhalo of mass 10^6-10^8 M_sun, or by interactions with giant molecular clouds, the Galactic bar, or spiral arms? | Were the off-stream spur, density gap, and cocoon structures observed in the thin globular cluster stream GD-1 (and Palomar 5) produced by the gravitational impulse of a dark, starless dark matter subhalo of mass 10^6-10^8 M_sun, or by interactions with giant molecular clouds, the Galactic bar, or spiral arms? Highligh... | milky_way_local_group_near_field | 5 | Milky Way, Local Group, and Near-Field Cosmology | stellar_streams_halo_substructure_and_accretion_history | [] | model_discrimination | [
"milky_way_component",
"dark_sector",
"stellar_population"
] | population_level | Astrophysical systems in stellar streams halo substructure and accretion history | [
"pc",
"kpc"
] | [
{
"name": "milky_way_assembly_history",
"redshift_min": 0,
"redshift_max": 4,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.2
}
] | [
"optical",
"near_ir"
] | [
"Gaia",
"SDSS-V",
"APOGEE",
"GALAH",
"WEAVE"
] | [
"Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial velocity) from Gaia",
"High-resolution stellar photospheric elemental abundances ([Fe/H], [alpha/Fe], r- and s-process ratios)",
"Cold stellar stream track density profiles, velocity dispersions, and off-stream spurs"
] | [
"Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial mass M_200",
"Accretion history of disrupted progenitor dwarfs (Gaia-Sausage-Enceladus, Sagittarius, Kraken)",
"Inner dark matter density slope d ln rho / d ln r in Local Group dwarf spheroidals"
] | [
"Three-dimensional interstellar dust extinction in the Galactic plane and inner bulge",
"Binary star orbital motion inflating apparent velocity dispersions in ultra-faint dwarfs"
] | [
"Non-LTE and 3D convective photospheric abundance corrections across giant and dwarf stars",
"Gaia parallax zero-point spatial variations and crowding in globular cluster cores"
] | [
"Orbital velocity anisotropy beta(r) vs inner dark matter cusp/core density profile",
"Secular radial migration vs merger-induced heating in the Galactic disk"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Milky Way, Local Group, and Near-Field Cosmology community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in stellar streams halo substructure and a from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial. | Current observations from Gaia, SDSS-V, APOGEE constrain Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial , but systematic uncertainties in Non-LTE and 3D convective photospheric abundance corrections across gi prevent a definitive resolution. | [
"Baseline astrophysical mechanism in stellar streams halo substructure and accretion history constrained by Gaia, SDSS-V",
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{
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{
"source_id": "SRC-AST-011263",
"citation": "Hilmi et al. (2024, arXiv (astro-ph.GA))",
"support_t... | [
"UAST-000007",
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] | null | [] | [
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000046 | UAST-000046 | uast-000046-origin-and-energy-source-of-the-fermi-gamma-ray-and-erosita-x-ray-bubbles | Origin and Energy Source of the Fermi Gamma-Ray and eROSITA X-Ray Bubbles | Were the bipolar 10-kpc Fermi gamma-ray bubbles and surrounding 14-kpc eROSITA X-ray bubbles launched by a Seyfert-like AGN jet or wind outburst from Sgr A* a few Myr ago, or by cumulative cosmic-ray and superwind feedback from nuclear starburst activity in the Central Molecular Zone? | Were the bipolar 10-kpc Fermi gamma-ray bubbles and surrounding 14-kpc eROSITA X-ray bubbles launched by a Seyfert-like AGN jet or wind outburst from Sgr A* a few Myr ago, or by cumulative cosmic-ray and superwind feedback from nuclear starburst activity in the Central Molecular Zone? | Were the bipolar 10-kpc Fermi gamma-ray bubbles and surrounding 14-kpc eROSITA X-ray bubbles launched by a Seyfert-like AGN jet or wind outburst from Sgr A* a few Myr ago, or by cumulative cosmic-ray and superwind feedback from nuclear starburst activity in the Central Molecular Zone? Highlighted as a key community res... | milky_way_local_group_near_field | 5 | Milky Way, Local Group, and Near-Field Cosmology | galactic_center_and_fermi_erosita_bubbles | [] | origin | [
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Milky Way, Local Group, and Near-Field Cosmology community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in galactic center and fermi erosita bubbl from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial. | Current observations from Gaia, SDSS-V, APOGEE constrain Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial , but systematic uncertainties in Non-LTE and 3D convective photospheric abundance corrections across gi prevent a definitive resolution. | [
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{
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{
"source_id": "SRC-AST-011022",
"citation": "Zhang et al. (2025, arXiv (astro-ph.GA))... | [
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000005). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000047 | UAST-000047 | uast-000047-first-generation-population-iii-survivor-stars-vs-pair-instability-supernova-chemical | First-Generation Population III Survivor Stars vs Pair-Instability Supernova Chemical Signatures in Ultra-Metal-Poor Halo Stars | Why have no zero-metallicity Population III low-mass survivor stars been found in the Galactic halo down to [Fe/H] < -7, and do carbon-enhanced extremely metal-poor (CEMP-no) stars reflect enrichment by faint core-collapse fallback supernovae, rapidly rotating spinstars, or pair-instability supernovae from massive firs... | Why have no zero-metallicity Population III low-mass survivor stars been found in the Galactic halo down to [Fe/H] < -7, and do carbon-enhanced extremely metal-poor (CEMP-no) stars reflect enrichment by faint core-collapse fallback supernovae, rapidly rotating spinstars, or pair-instability supernovae from massive firs... | Why have no zero-metallicity Population III low-mass survivor stars been found in the Galactic halo down to [Fe/H] < -7, and do carbon-enhanced extremely metal-poor (CEMP-no) stars reflect enrichment by faint core-collapse fallback supernovae, rapidly rotating spinstars, or pair-instability supernovae from massive firs... | milky_way_local_group_near_field | 5 | Milky Way, Local Group, and Near-Field Cosmology | galactic_archaeology_and_chemical_evolution | [] | origin | [
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"stellar_population",
"milky_way_component"
] | population_level | Astrophysical systems in galactic archaeology and chemical evolution | [
"pc",
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{
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Milky Way, Local Group, and Near-Field Cosmology community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in galactic archaeology and chemical evolu from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Six-dimensional stellar phase-space coordinates (parallax, proper motion, radial. | Current observations from Gaia, SDSS-V, APOGEE constrain Milky Way gravitational potential Phi(R, z), dark halo triaxiality, and total virial , but systematic uncertainties in Non-LTE and 3D convective photospheric abundance corrections across gi prevent a definitive resolution. | [
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{
"source_id": "SRC-AST-000003",
"support_type": "direct_open_question",
"locator": "Section 3.2: First Stars and Galactic Archaeology, p. 48",
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},
{
"source_id": "SRC-AST-017511",
"citation": "Hansen et al. (2015, arXiv (astro-ph.SR))",
"support_type": "e... | [
"UAST-000007",
"UAST-019211",
"UAST-018190",
"UAST-013546"
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"milky_way_local_group_near_field",
"galactic_archaeology_and_chemical_evolution",
"Population_III",
"CEMP_stars",
"pair_instability_supernovae",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000003). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000048 | UAST-000048 | uast-000048-magnetically-subcritical-vs-turbulent-regulation-of-molecular-cloud-core-collapse | Magnetically Subcritical vs Turbulent Regulation of Molecular Cloud Core Collapse | What is the statistical distribution of the mass-to-magnetic-flux ratio mu_Phi across prestellar molecular cloud cores from 0.01 to 1 pc, and is the low cosmic star formation efficiency per free-fall time (epsilon_ff ~ 0.01) primarily regulated by supersonic magnetohydrodynamic turbulence, ambipolar diffusion of strong... | What is the statistical distribution of the mass-to-magnetic-flux ratio mu_Phi across prestellar molecular cloud cores from 0.01 to 1 pc, and is the low cosmic star formation efficiency per free-fall time (epsilon_ff ~ 0.01) primarily regulated by supersonic magnetohydrodynamic turbulence, ambipolar diffusion of strong... | What is the statistical distribution of the mass-to-magnetic-flux ratio mu_Phi across prestellar molecular cloud cores from 0.01 to 1 pc, and is the low cosmic star formation efficiency per free-fall time (epsilon_ff ~ 0.01) primarily regulated by supersonic magnetohydrodynamic turbulence, ambipolar diffusion of strong... | ism_star_formation_astrochemistry | 6 | Interstellar Medium, Star Formation, and Astrochemistry | ism_phases_turbulence_and_magnetic_fields | [] | mechanism | [
"interstellar_medium",
"star"
] | population_level | Astrophysical systems in ism phases turbulence and magnetic fields | [
"au",
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{
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Interstellar Medium, Star Formation, and Astrochemistry community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in ism phases turbulence and magnetic fiel from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Millimeter rotational molecular line spectra (CO, N2H+, HCN, HCO+, CH3OH, COMs) . | Current observations from ALMA, JWST, NOEMA constrain Magnetic field strength B, mass-to-flux ratio mu_Phi, and sonic Mach number M_s in mo, but systematic uncertainties in CO-to-H2 conversion factor X_CO and dust opacity spectral index beta v prevent a definitive resolution. | [
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{
"source_id": "SRC-AST-000007",
"support_type": "direct_open_question",
"locator": "Section 2.1: Interstellar Medium and Star Formation Physics, p. 12",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-032610",
"citation": "Bertram et al. (2011, arXiv (astro-ph.SR))",
"suppor... | [
"UAST-000008",
"UAST-032884",
"UAST-015433",
"UAST-001511"
] | null | [] | [
"ism_star_formation_astrochemistry",
"ism_phases_turbulence_and_magnetic_fields",
"molecular_clouds",
"star_formation_efficiency",
"magnetic_fields",
"MHD_turbulence"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000007). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000049 | UAST-000049 | uast-000049-origin-of-the-universal-0-1-pc-characteristic-width-of-interstellar-molecular-filamen | Origin of the Universal ~0.1 pc Characteristic Width of Interstellar Molecular Filaments | Do dense molecular filaments in nearby star-forming clouds genuinely possess a quasi-universal characteristic inner width of ~0.1 pc set by the sonic scale of supersonic MHD turbulence or ion-neutral friction, or is this apparent scale invariance partially an artifact of radiative transfer, dust temperature gradients, ... | Do dense molecular filaments in nearby star-forming clouds genuinely possess a quasi-universal characteristic inner width of ~0.1 pc set by the sonic scale of supersonic MHD turbulence or ion-neutral friction, or is this apparent scale invariance partially an artifact of radiative transfer, dust temperature gradients, ... | Do dense molecular filaments in nearby star-forming clouds genuinely possess a quasi-universal characteristic inner width of ~0.1 pc set by the sonic scale of supersonic MHD turbulence or ion-neutral friction, or is this apparent scale invariance partially an artifact of radiative transfer, dust temperature gradients, ... | ism_star_formation_astrochemistry | 6 | Interstellar Medium, Star Formation, and Astrochemistry | molecular_clouds_cores_and_star_formation_laws | [] | mechanism | [
"interstellar_medium"
] | population_level | Astrophysical systems in molecular clouds cores and star formation laws | [
"pc"
] | [
{
"name": "present_day_and_galactic_ism",
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"redshift_max": 2,
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}
] | [
"far_ir",
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"Star formation efficiency per free-fall time epsilon_ff and core/stellar initial mass function",
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"Excitation temperature and critical density biases across molecular line tracers"
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"Molecular freeze-out onto cold dust grains in high-density prestellar cores"
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"Dust temperature gradients vs column density structure along the line of sight",
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Interstellar Medium, Star Formation, and Astrochemistry community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in molecular clouds cores and star formati from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Millimeter rotational molecular line spectra (CO, N2H+, HCN, HCO+, CH3OH, COMs) . | Current observations from ALMA, JWST, NOEMA constrain Magnetic field strength B, mass-to-flux ratio mu_Phi, and sonic Mach number M_s in mo, but systematic uncertainties in CO-to-H2 conversion factor X_CO and dust opacity spectral index beta v prevent a definitive resolution. | [
"Baseline astrophysical mechanism in molecular clouds cores and star formation laws constrained by ALMA, JWST",
"Alternative non-equilibrium, feedback, or multi-component physical model for Origin of the Universal ~0.1 pc Characteristic Width of Interstellar M"
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{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Appendix E: Stars, the Sun, and Stellar Populations, p. E-11",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-014961",
"citation": "Hennebelle et al. (2013, arXiv (astro-ph.GA))",
"support_t... | [
"UAST-000008",
"UAST-016934",
"UAST-025550",
"UAST-015388"
] | null | [] | [
"ism_star_formation_astrochemistry",
"molecular_clouds_cores_and_star_formation_laws",
"molecular_filaments",
"filament_width",
"sonic_scale",
"Herschel_ALMA"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000050 | UAST-000050 | uast-000050-environmental-universality-vs-top-heavy-bottom-heavy-variation-of-the-stellar-initial | Environmental Universality vs Top-Heavy / Bottom-Heavy Variation of the Stellar Initial Mass Function | Does the stellar initial mass function deviate systematically from the Milky Way Chabrier/Kroupa form toward a bottom-heavy slope in the high-velocity-dispersion cores of massive early-type galaxies and a top-heavy slope in low-metallicity or extreme starburst environments? | Does the stellar initial mass function deviate systematically from the Milky Way Chabrier/Kroupa form toward a bottom-heavy slope in the high-velocity-dispersion cores of massive early-type galaxies and a top-heavy slope in low-metallicity or extreme starburst environments? | Does the stellar initial mass function deviate systematically from the Milky Way Chabrier/Kroupa form toward a bottom-heavy slope in the high-velocity-dispersion cores of massive early-type galaxies and a top-heavy slope in low-metallicity or extreme starburst environments? Highlighted as a key community research quest... | ism_star_formation_astrochemistry | 6 | Interstellar Medium, Star Formation, and Astrochemistry | stellar_initial_mass_function_and_clustered_star_formation | [] | population_evolution | [
"stellar_population",
"interstellar_medium",
"galaxy"
] | population_level | Astrophysical systems in stellar initial mass function and clustered star formation | [
"pc",
"kpc"
] | [
{
"name": "present_day_and_galactic_ism",
"redshift_min": 0,
"redshift_max": 2,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 10.4
}
] | [
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"near_ir",
"mm_submm"
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"ALMA",
"JWST",
"NOEMA",
"VLA",
"ngVLA"
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"Millimeter rotational molecular line spectra (CO, N2H+, HCN, HCO+, CH3OH, COMs) and Zeeman splitting",
"Submillimeter polarized thermal dust continuum emission and mid-IR ice absorption bands",
"Optical/NIR diffuse interstellar absorption band profiles and PAH mid-IR emission features"
] | [
"Magnetic field strength B, mass-to-flux ratio mu_Phi, and sonic Mach number M_s in molecular cores",
"Star formation efficiency per free-fall time epsilon_ff and core/stellar initial mass function",
"Gas-phase and grain-surface reaction rates, deuteration fractions, and dust grain size distributions"
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"Interferometric spatial filtering of extended diffuse emission in molecular clouds",
"Excitation temperature and critical density biases across molecular line tracers"
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"CO-to-H2 conversion factor X_CO and dust opacity spectral index beta variations",
"Molecular freeze-out onto cold dust grains in high-density prestellar cores"
] | [
"Dust temperature gradients vs column density structure along the line of sight",
"Grain-surface radical recombination vs gas-phase ion-molecule synthesis of COMs"
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UAST-000051 | UAST-000051 | uast-000051-monolithic-turbulent-core-accretion-vs-competitive-filamentary-accretion-in-massive-s | Monolithic Turbulent Core Accretion vs Competitive Filamentary Accretion in Massive Star Formation (> 20 M_sun) | Do massive stars (M_* > 20-100 M_sun) assemble primarily from isolated, virialized, magnetically supported turbulent massive prestellar cores, or through hierarchical, clump-fed competitive accretion along converging hub-filament systems where massive protostars grow concurrently with cluster assembly? | Do massive stars (M_* > 20-100 M_sun) assemble primarily from isolated, virialized, magnetically supported turbulent massive prestellar cores, or through hierarchical, clump-fed competitive accretion along converging hub-filament systems where massive protostars grow concurrently with cluster assembly? | Do massive stars (M_* > 20-100 M_sun) assemble primarily from isolated, virialized, magnetically supported turbulent massive prestellar cores, or through hierarchical, clump-fed competitive accretion along converging hub-filament systems where massive protostars grow concurrently with cluster assembly? Highlighted as a... | ism_star_formation_astrochemistry | 6 | Interstellar Medium, Star Formation, and Astrochemistry | massive_star_formation_and_feedback | [] | model_discrimination | [
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"support_typ... | [
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"massive_star_formation_and_feedback",
"massive_star_formation",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000008). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000052 | UAST-000052 | uast-000052-survival-destruction-and-in-situ-grain-growth-of-interstellar-dust-in-the-multiphase | Survival, Destruction, and In-Situ Grain Growth of Interstellar Dust in the Multiphase ISM | Given that supernova shock sputtering destroys interstellar silicate and carbonaceous dust grains on timescales of ~100-300 Myr—much shorter than their injection timescale from asymptotic giant branch stars and core-collapse supernovae—what physical and chemical mechanisms enable rapid dust grain accretion and coagulat... | Given that supernova shock sputtering destroys interstellar silicate and carbonaceous dust grains on timescales of ~100-300 Myr—much shorter than their injection timescale from asymptotic giant branch stars and core-collapse supernovae—what physical and chemical mechanisms enable rapid dust grain accretion and coagulat... | Given that supernova shock sputtering destroys interstellar silicate and carbonaceous dust grains on timescales of ~100-300 Myr—much shorter than their injection timescale from asymptotic giant branch stars and core-collapse supernovae—what physical and chemical mechanisms enable rapid dust grain accretion and coagulat... | ism_star_formation_astrochemistry | 6 | Interstellar Medium, Star Formation, and Astrochemistry | interstellar_dust_pahs_and_ices | [] | mechanism | [
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{
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"support_type": "... | [
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000053 | UAST-000053 | uast-000053-gas-phase-vs-ice-mantle-radical-recombination-pathways-for-interstellar-complex-organ | Gas-Phase vs Ice-Mantle Radical Recombination Pathways for Interstellar Complex Organic Molecules in Cold Prestellar Cores | How are complex organic molecules (COMs such as CH3OH, CH3OCHO, and CH3OCH3) synthesized and desorbed into the gas phase in cold (T ~ 10 K), UV-shielded prestellar cores where thermal diffusion and thermal desorption of heavy radicals on water-ice grain mantles are exponentially suppressed? | How are complex organic molecules (COMs such as CH3OH, CH3OCHO, and CH3OCH3) synthesized and desorbed into the gas phase in cold (T ~ 10 K), UV-shielded prestellar cores where thermal diffusion and thermal desorption of heavy radicals on water-ice grain mantles are exponentially suppressed? | How are complex organic molecules (COMs such as CH3OH, CH3OCHO, and CH3OCH3) synthesized and desorbed into the gas phase in cold (T ~ 10 K), UV-shielded prestellar cores where thermal diffusion and thermal desorption of heavy radicals on water-ice grain mantles are exponentially suppressed? Highlighted as a key communi... | ism_star_formation_astrochemistry | 6 | Interstellar Medium, Star Formation, and Astrochemistry | astrochemistry_and_complex_organic_molecules | [] | mechanism | [
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000008). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000054 | UAST-000054 | uast-000054-internal-angular-momentum-transport-efficiency-in-red-giant-and-subgiant-stars | Internal Angular Momentum Transport Efficiency in Red Giant and Subgiant Stars | What magnetohydrodynamic or wave-driven physical mechanism (such as the Tayler-Spruit dynamo, azimuthal magnetorotational instability, or mixed gravito-inertial waves) transports angular momentum between contracting helium cores and expanding convective envelopes in subgiants and red giants, explaining core rotation ra... | What magnetohydrodynamic or wave-driven physical mechanism (such as the Tayler-Spruit dynamo, azimuthal magnetorotational instability, or mixed gravito-inertial waves) transports angular momentum between contracting helium cores and expanding convective envelopes in subgiants and red giants, explaining core rotation ra... | What magnetohydrodynamic or wave-driven physical mechanism (such as the Tayler-Spruit dynamo, azimuthal magnetorotational instability, or mixed gravito-inertial waves) transports angular momentum between contracting helium cores and expanding convective envelopes in subgiants and red giants, explaining core rotation ra... | stars_stellar_populations_evolution | 7 | Stars, Stellar Populations, and Stellar Evolution | stellar_interiors_convection_rotation_and_magnetism | [] | mechanism | [
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] | population_level | Astrophysical systems in stellar interiors convection rotation and magnetism | [
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{
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000055 | UAST-000055 | uast-000055-continuum-driven-super-eddington-eruptions-vs-binary-interaction-in-luminous-blue-var | Continuum-Driven Super-Eddington Eruptions vs Binary Interaction in Luminous Blue Variables and Pre-Supernova Mass Loss | Are giant mass-loss eruptions in Luminous Blue Variables (such as Eta Carinae's 19th-century Great Eruption shedding > 10 M_sun) and dense circumstellar shells around Type IIn/Ibn supernovae driven by single-star super-Eddington continuum/wave-heated envelope instabilities or by binary inspiral, common-envelope ejectio... | Are giant mass-loss eruptions in Luminous Blue Variables (such as Eta Carinae's 19th-century Great Eruption shedding > 10 M_sun) and dense circumstellar shells around Type IIn/Ibn supernovae driven by single-star super-Eddington continuum/wave-heated envelope instabilities or by binary inspiral, common-envelope ejectio... | Are giant mass-loss eruptions in Luminous Blue Variables (such as Eta Carinae's 19th-century Great Eruption shedding > 10 M_sun) and dense circumstellar shells around Type IIn/Ibn supernovae driven by single-star super-Eddington continuum/wave-heated envelope instabilities or by binary inspiral, common-envelope ejectio... | stars_stellar_populations_evolution | 7 | Stars, Stellar Populations, and Stellar Evolution | massive_stars_winds_and_mass_loss | [] | mechanism | [
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] | population_level | Astrophysical systems in massive stars winds and mass loss | [
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{
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000056 | UAST-000056 | uast-000056-common-envelope-binding-energy-efficiency-alpha-ce-and-post-inspiral-orbital-separati | Common-Envelope Binding Energy Efficiency alpha_CE and Post-Inspiral Orbital Separation | What is the quantitative energy budget—including orbital energy release, H/He recombination energy, enthalpy, and radiation-hydrodynamic outflows—that determines whether a binary star survives a common-envelope episode as a close post-common-envelope binary or merges completely? | What is the quantitative energy budget—including orbital energy release, H/He recombination energy, enthalpy, and radiation-hydrodynamic outflows—that determines whether a binary star survives a common-envelope episode as a close post-common-envelope binary or merges completely? | What is the quantitative energy budget—including orbital energy release, H/He recombination energy, enthalpy, and radiation-hydrodynamic outflows—that determines whether a binary star survives a common-envelope episode as a close post-common-envelope binary or merges completely? Highlighted as a key community research ... | stars_stellar_populations_evolution | 7 | Stars, Stellar Populations, and Stellar Evolution | binary_and_multiple_star_evolution | [] | mechanism | [
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{
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{
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] | null | [] | [
"stars_stellar_populations_evolution",
"binary_and_multiple_star_evolution",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000006). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000057 | UAST-000057 | uast-000057-the-red-supergiant-problem-and-explodability-threshold-of-17-25-m-sun-core-collapse-p | The Red Supergiant Problem and Explodability Threshold of 17-25 M_sun Core-Collapse Progenitors | Why have pre-explosion archival imaging surveys (HST/JWST) detected almost no Type II-P supernova progenitors with initial masses above ~17-18 M_sun despite red supergiants existing up to ~25-30 M_sun, and do these higher-mass cores collapse directly to black holes via failed supernovae or experience severe pre-explosi... | Why have pre-explosion archival imaging surveys (HST/JWST) detected almost no Type II-P supernova progenitors with initial masses above ~17-18 M_sun despite red supergiants existing up to ~25-30 M_sun, and do these higher-mass cores collapse directly to black holes via failed supernovae or experience severe pre-explosi... | Why have pre-explosion archival imaging surveys (HST/JWST) detected almost no Type II-P supernova progenitors with initial masses above ~17-18 M_sun despite red supergiants existing up to ~25-30 M_sun, and do these higher-mass cores collapse directly to black holes via failed supernovae or experience severe pre-explosi... | stars_stellar_populations_evolution | 7 | Stars, Stellar Populations, and Stellar Evolution | late_stages_supernovae_progenitors_and_remnants | [] | tension_resolution | [
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"transient",
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] | population_level | Astrophysical systems in late stages supernovae progenitors and remnants | [
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{
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{
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"stars_stellar_populations_evolution",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000058 | UAST-000058 | uast-000058-convective-core-overshooting-calibration-across-main-sequence-intermediate-and-high-m | Convective Core Overshooting Calibration Across Main-Sequence Intermediate- and High-Mass Stars | How does the convective core boundary mixing and overshooting length scale alpha_ov vary with stellar mass, rotation rate, and metallicity across 1.2 <= M/M_sun <= 30 as measured by gravity-mode period spacings in gamma Doradus / SPB stars and detached eclipsing binaries? | How does the convective core boundary mixing and overshooting length scale alpha_ov vary with stellar mass, rotation rate, and metallicity across 1.2 <= M/M_sun <= 30 as measured by gravity-mode period spacings in gamma Doradus / SPB stars and detached eclipsing binaries? | How does the convective core boundary mixing and overshooting length scale alpha_ov vary with stellar mass, rotation rate, and metallicity across 1.2 <= M/M_sun <= 30 as measured by gravity-mode period spacings in gamma Doradus / SPB stars and detached eclipsing binaries? Highlighted as a key community research questio... | stars_stellar_populations_evolution | 7 | Stars, Stellar Populations, and Stellar Evolution | stellar_populations_clusters_and_asteroseismology | [] | value_or_bound | [
"star",
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] | population_level | Astrophysical systems in stellar populations clusters and asteroseismology | [
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{
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{
"source_id": "SRC-AST-017197",
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... | [
"UAST-000009",
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] | null | [] | [
"stars_stellar_populations_evolution",
"stellar_populations_clusters_and_asteroseismology",
"convective_overshooting",
"gravity_modes",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000002). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000059 | UAST-000059 | uast-000059-clumping-factor-and-metallicity-scaling-of-line-driven-winds-in-o-type-and-wolf-rayet | Clumping Factor and Metallicity Scaling of Line-Driven Winds in O-Type and Wolf-Rayet Stars | What is the exact wind clumping factor f_cl and porosity-corrected mass-loss rate scaling dM/dt ~ Z^m for massive O-type, Wolf-Rayet, and stripped helium stars at sub-SMC metallicities (Z <= 0.1 Z_sun), and how strongly does reduced wind mass loss preserve high core masses and angular momentum in the early universe? | What is the exact wind clumping factor f_cl and porosity-corrected mass-loss rate scaling dM/dt ~ Z^m for massive O-type, Wolf-Rayet, and stripped helium stars at sub-SMC metallicities (Z <= 0.1 Z_sun), and how strongly does reduced wind mass loss preserve high core masses and angular momentum in the early universe? | What is the exact wind clumping factor f_cl and porosity-corrected mass-loss rate scaling dM/dt ~ Z^m for massive O-type, Wolf-Rayet, and stripped helium stars at sub-SMC metallicities (Z <= 0.1 Z_sun), and how strongly does reduced wind mass loss preserve high core masses and angular momentum in the early universe? Hi... | stars_stellar_populations_evolution | 7 | Stars, Stellar Populations, and Stellar Evolution | massive_stars_winds_and_mass_loss | [] | value_or_bound | [
"star"
] | population_level | Astrophysical systems in massive stars winds and mass loss | [
"1000km_to_rsun",
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{
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{
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{
"source_id": "SRC-AST-015860",
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"UAST-000009",
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] | null | [] | [
"stars_stellar_populations_evolution",
"massive_stars_winds_and_mass_loss",
"massive_star_winds",
"wind_clumping",
"low_metallicity",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000060 | UAST-000060 | uast-000060-merger-and-crystallization-origin-of-highly-magnetized-massive-white-dwarfs | Merger and Crystallization Origin of Highly Magnetized Massive White Dwarfs | What fraction of highly magnetized white dwarfs (B ~ 10^6-10^9 G, which are systematically more massive than non-magnetic white dwarfs) originate from double-degenerate mergers or common-envelope dynamos versus convective dynamos driven by carbon-oxygen core crystallization and phase separation during cooling? | What fraction of highly magnetized white dwarfs (B ~ 10^6-10^9 G, which are systematically more massive than non-magnetic white dwarfs) originate from double-degenerate mergers or common-envelope dynamos versus convective dynamos driven by carbon-oxygen core crystallization and phase separation during cooling? | What fraction of highly magnetized white dwarfs (B ~ 10^6-10^9 G, which are systematically more massive than non-magnetic white dwarfs) originate from double-degenerate mergers or common-envelope dynamos versus convective dynamos driven by carbon-oxygen core crystallization and phase separation during cooling? Highligh... | compact_objects_accretion_high_energy | 8 | Compact Objects, Accretion, and High-Energy Astrophysics | white_dwarfs_and_thermonuclear_transients | [] | origin | [
"compact_object",
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] | population_level | Astrophysical systems in white dwarfs and thermonuclear transients | [
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"Baseline astrophysical mechanism in white dwarfs and thermonuclear transients constrained by NICER, IXPE",
"Alternative non-equilibrium, feedback, or multi-component physical model for Merger and Crystallization Origin of Highly Magnetized Massive White D"
] | [
"High-significance multi-wavelength or dynamical measurement of Energy-resolved X-ray pulse profiles, relativistic Fe K-alpha reflection spectra, and X-ra using NICER, IXPE, XRISM.",
"Breaking the model degeneracy between Quark-matter phase transition vs hyperon softening in neutron star mass-radius curves to bet... | Resolving this question in Compact Objects, Accretion, and High-Energy Astrophysics is essential for calibrating Cold supranuclear dense matter pressure-density relation P(epsilon), neutron sta and testing fundamental astrophysical theory. | General relativistic compact objects, supranuclear dense matter equations of state, pulsar magnetospheric electrodynamics, and black hole accretion disk/jet magnetohydrodynamics. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
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{
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"support_type... | [
"UAST-000010",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000061 | UAST-000061 | uast-000061-coherent-radio-pulsar-emission-mechanism-and-pair-cascade-microphysics-in-the-polar-c | Coherent Radio Pulsar Emission Mechanism and Pair-Cascade Microphysics in the Polar Cap vs Light Cylinder | What plasma microphysics generates the extreme brightness temperatures (T_b > 10^25-10^30 K) and orthogonal polarization modes of coherent pulsar radio emission, and what fraction originates from non-stationary spark-driven pair cascades above the polar cap versus magnetic reconnection in the current sheet beyond the l... | What plasma microphysics generates the extreme brightness temperatures (T_b > 10^25-10^30 K) and orthogonal polarization modes of coherent pulsar radio emission, and what fraction originates from non-stationary spark-driven pair cascades above the polar cap versus magnetic reconnection in the current sheet beyond the l... | What plasma microphysics generates the extreme brightness temperatures (T_b > 10^25-10^30 K) and orthogonal polarization modes of coherent pulsar radio emission, and what fraction originates from non-stationary spark-driven pair cascades above the polar cap versus magnetic reconnection in the current sheet beyond the l... | compact_objects_accretion_high_energy | 8 | Compact Objects, Accretion, and High-Energy Astrophysics | neutron_stars_pulsars_and_magnetars | [] | mechanism | [
"compact_object"
] | population_level | Astrophysical systems in neutron stars pulsars and magnetars | [
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{
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{
"source_id": "SRC-AST-012027",
"citation": "Lobato et al. (2015, Astronomy Journal)",
"support_type": ... | [
"UAST-000010",
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] | null | [] | [
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"neutron_stars_pulsars_and_magnetars",
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UAST-000062 | UAST-000062 | uast-000062-superfluid-vortex-unpinning-vs-crustal-cracking-in-pulsar-timing-glitches | Superfluid Vortex Unpinning vs Crustal Cracking in Pulsar Timing Glitches | Are large spin-up glitches (Delta nu / nu ~ 10^-6) and post-glitch exponential recoveries in young pulsars like Vela triggered purely by collective unpinning of quantized neutron superfluid vortices in the inner crust and outer core, or by hydro-elastic crustal fractures and magnetospheric state changes? | Are large spin-up glitches (Delta nu / nu ~ 10^-6) and post-glitch exponential recoveries in young pulsars like Vela triggered purely by collective unpinning of quantized neutron superfluid vortices in the inner crust and outer core, or by hydro-elastic crustal fractures and magnetospheric state changes? | Are large spin-up glitches (Delta nu / nu ~ 10^-6) and post-glitch exponential recoveries in young pulsars like Vela triggered purely by collective unpinning of quantized neutron superfluid vortices in the inner crust and outer core, or by hydro-elastic crustal fractures and magnetospheric state changes? Highlighted as... | compact_objects_accretion_high_energy | 8 | Compact Objects, Accretion, and High-Energy Astrophysics | neutron_stars_pulsars_and_magnetars | [] | mechanism | [
"compact_object"
] | population_level | Astrophysical systems in neutron stars pulsars and magnetars | [
"km_to_1000km"
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{
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"High-precision radio pulsar times of arrival (TOAs), dispersion/rotation measures, and glitch spin-up steps",
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{
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{
"source_id": "SRC-AST-019187",
"citation": "Deepthi et al. (2025, J.Subatomic Part.Cosmol.)",
"support_type... | [
"UAST-000010",
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"compact_objects_accretion_high_energy",
"neutron_stars_pulsars_and_magnetars",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000004). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000063 | UAST-000063 | uast-000063-black-hole-spin-alignment-vs-discrepancy-between-continuum-fitting-relativistic-fe-k | Black Hole Spin Alignment vs Discrepancy Between Continuum Fitting, Relativistic Fe K-alpha Reflection, and Gravitational Waves | Why do X-ray reflection and thermal continuum-fitting measurements in stellar-mass black hole X-ray binaries frequently infer high dimensionless spins (a_* > 0.7-0.95), whereas LIGO-Virgo-KAGRA binary black hole mergers exhibit a distribution centered at low effective spins (chi_eff ~ 0.05-0.2)? | Why do X-ray reflection and thermal continuum-fitting measurements in stellar-mass black hole X-ray binaries frequently infer high dimensionless spins (a_* > 0.7-0.95), whereas LIGO-Virgo-KAGRA binary black hole mergers exhibit a distribution centered at low effective spins (chi_eff ~ 0.05-0.2)? | Why do X-ray reflection and thermal continuum-fitting measurements in stellar-mass black hole X-ray binaries frequently infer high dimensionless spins (a_* > 0.7-0.95), whereas LIGO-Virgo-KAGRA binary black hole mergers exhibit a distribution centered at low effective spins (chi_eff ~ 0.05-0.2)? Highlighted as a key co... | compact_objects_accretion_high_energy | 8 | Compact Objects, Accretion, and High-Energy Astrophysics | stellar_mass_black_holes_and_x_ray_binaries | [] | tension_resolution | [
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] | population_level | Astrophysical systems in stellar mass black holes and x ray binaries | [
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{
"source_id": "SRC-AST-022337",
"citation": "Larsen et al. (2025, Astrophysics & Astronomy Literature... | [
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] | null | [] | [
"compact_objects_accretion_high_energy",
"stellar_mass_black_holes_and_x_ray_binaries",
"black_hole_spin",
"X_ray_reflection",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000005). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000064 | UAST-000064 | uast-000064-physical-trigger-of-state-transitions-and-low-frequency-qpos-in-black-hole-x-ray-bina | Physical Trigger of State Transitions and Low-Frequency QPOs in Black Hole X-Ray Binaries | What physical instability triggers the hard-to-soft spectral state transition in black hole X-ray binaries, and are Type-C low-frequency quasi-periodic oscillations (0.1-30 Hz) caused by Lense-Thirring relativistic precession of a hot inner accretion flow or by magneto-acoustic oscillations of the disk-corona boundary? | What physical instability triggers the hard-to-soft spectral state transition in black hole X-ray binaries, and are Type-C low-frequency quasi-periodic oscillations (0.1-30 Hz) caused by Lense-Thirring relativistic precession of a hot inner accretion flow or by magneto-acoustic oscillations of the disk-corona boundary? | What physical instability triggers the hard-to-soft spectral state transition in black hole X-ray binaries, and are Type-C low-frequency quasi-periodic oscillations (0.1-30 Hz) caused by Lense-Thirring relativistic precession of a hot inner accretion flow or by magneto-acoustic oscillations of the disk-corona boundary?... | compact_objects_accretion_high_energy | 8 | Compact Objects, Accretion, and High-Energy Astrophysics | accretion_disks_winds_and_coronae | [] | mechanism | [
"compact_object"
] | population_level | Astrophysical systems in accretion disks winds and coronae | [
"km_to_1000km"
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{
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"NICER",
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"XRISM",
"Chandra",
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"Binary neutron star gravitational-wave tidal deformability Lambda_tilde ... | [
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] | [
"Quark-matter phase transition vs hyperon softening in neutron star mass-radius curves",
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"Baseline astrophysical mechanism in accretion disks winds and coronae constrained by NICER, IXPE",
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{
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"citation": "Nathan et al. (2022, arXiv (astro-ph.HE))",
"supp... | [
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"Lense_Thirring_precession",
"X_ray_binaries",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000005). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000065 | UAST-000065 | uast-000065-magnetic-energy-dissipation-and-particle-acceleration-at-the-termination-shock-of-pul | Magnetic Energy Dissipation and Particle Acceleration at the Termination Shock of Pulsar Wind Nebulae | How is the Poynting-flux-dominated relativistic magnetohydrodynamic outflow from a pulsar (magnetization sigma >> 1 at the light cylinder) converted into a particle-dominated plasma (sigma << 1) upstream of or at the termination shock in pulsar wind nebulae such as the Crab Nebula (the sigma problem), and how do Crab g... | How is the Poynting-flux-dominated relativistic magnetohydrodynamic outflow from a pulsar (magnetization sigma >> 1 at the light cylinder) converted into a particle-dominated plasma (sigma << 1) upstream of or at the termination shock in pulsar wind nebulae such as the Crab Nebula (the sigma problem), and how do Crab g... | How is the Poynting-flux-dominated relativistic magnetohydrodynamic outflow from a pulsar (magnetization sigma >> 1 at the light cylinder) converted into a particle-dominated plasma (sigma << 1) upstream of or at the termination shock in pulsar wind nebulae such as the Crab Nebula (the sigma problem), and how do Crab g... | compact_objects_accretion_high_energy | 8 | Compact Objects, Accretion, and High-Energy Astrophysics | relativistic_jets_and_pulsar_wind_nebulae | [] | mechanism | [
"compact_object",
"nonthermal_particle"
] | population_level | Astrophysical systems in relativistic jets and pulsar wind nebulae | [
"km_to_1000km",
"au",
"pc"
] | [
{
"name": "compact_object_populations",
"redshift_min": 0,
"redshift_max": 1.5,
"lookback_time_gyr_min": 0,
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] | [
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"IXPE",
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"XMM-Newton"
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"Radio pulsar beaming fraction and dispersion/scattering selection against Galactic Center pulsars",
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UAST-000066 | UAST-000066 | uast-000066-central-engine-vs-circumstellar-interaction-powering-superluminous-supernovae-slsne-i | Central Engine vs Circumstellar Interaction Powering Superluminous Supernovae (SLSNe-I) | Are hydrogen-poor superluminous supernovae (SLSNe-I, peak M < -21 mag) powered primarily by dipole spin-down of a nascent millisecond magnetar (P_0 ~ 1-5 ms, B ~ 10^14 G), fallback accretion onto a central black hole, or shock interaction with massive carbon-oxygen circumstellar shells ejected prior to explosion? | Are hydrogen-poor superluminous supernovae (SLSNe-I, peak M < -21 mag) powered primarily by dipole spin-down of a nascent millisecond magnetar (P_0 ~ 1-5 ms, B ~ 10^14 G), fallback accretion onto a central black hole, or shock interaction with massive carbon-oxygen circumstellar shells ejected prior to explosion? | Are hydrogen-poor superluminous supernovae (SLSNe-I, peak M < -21 mag) powered primarily by dipole spin-down of a nascent millisecond magnetar (P_0 ~ 1-5 ms, B ~ 10^14 G), fallback accretion onto a central black hole, or shock interaction with massive carbon-oxygen circumstellar shells ejected prior to explosion? Highl... | transients_gravitational_waves_multimessenger | 9 | Transients, Gravitational Waves, and Multi-Messenger Astronomy | supernovae_and_kilonovae | [] | model_discrimination | [
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UAST-000067 | UAST-000067 | uast-000067-prompt-gamma-ray-burst-emission-mechanism-photospheric-dissipation-vs-internal-shocks | Prompt Gamma-Ray Burst Emission Mechanism: Photospheric Dissipation vs Internal Shocks vs ICMART Magnetic Reconnection | Is the prompt MeV gamma-ray emission of gamma-ray bursts generated by sub-photospheric Comptonization in a baryon-loaded outflow, internal shocks in a variable hydrodynamic jet, or Poynting-flux-driven turbulent magnetic reconnection (ICMART) at large radii (R ~ 10^15 cm), as tested by MeV gamma-ray polarization and lo... | Is the prompt MeV gamma-ray emission of gamma-ray bursts generated by sub-photospheric Comptonization in a baryon-loaded outflow, internal shocks in a variable hydrodynamic jet, or Poynting-flux-driven turbulent magnetic reconnection (ICMART) at large radii (R ~ 10^15 cm), as tested by MeV gamma-ray polarization and lo... | Is the prompt MeV gamma-ray emission of gamma-ray bursts generated by sub-photospheric Comptonization in a baryon-loaded outflow, internal shocks in a variable hydrodynamic jet, or Poynting-flux-driven turbulent magnetic reconnection (ICMART) at large radii (R ~ 10^15 cm), as tested by MeV gamma-ray polarization and lo... | transients_gravitational_waves_multimessenger | 9 | Transients, Gravitational Waves, and Multi-Messenger Astronomy | gamma_ray_bursts_and_relativistic_explosions | [] | model_discrimination | [
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UAST-000068 | UAST-000068 | uast-000068-origin-of-long-period-18-60-minute-coherent-radio-transients-and-ultra-long-period-ma | Origin of Long-Period (18-60 Minute) Coherent Radio Transients and Ultra-Long-Period Magnetars | Are the recently discovered ultra-long-period coherent radio transients (with pulsation periods of 18 to 320 minutes, such as GLEAM-X J162759.5-523504.3 and GPM J1839-10) ultra-magnetized neutron stars / magnetars operating far below the canonical pulsar death line, or strongly magnetic isolated/binary white dwarf puls... | Are the recently discovered ultra-long-period coherent radio transients (with pulsation periods of 18 to 320 minutes, such as GLEAM-X J162759.5-523504.3 and GPM J1839-10) ultra-magnetized neutron stars / magnetars operating far below the canonical pulsar death line, or strongly magnetic isolated/binary white dwarf puls... | Are the recently discovered ultra-long-period coherent radio transients (with pulsation periods of 18 to 320 minutes, such as GLEAM-X J162759.5-523504.3 and GPM J1839-10) ultra-magnetized neutron stars / magnetars operating far below the canonical pulsar death line, or strongly magnetic isolated/binary white dwarf puls... | transients_gravitational_waves_multimessenger | 9 | Transients, Gravitational Waves, and Multi-Messenger Astronomy | fast_radio_bursts_and_coherent_radio_transients | [] | object_nature | [
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UAST-000069 | UAST-000069 | uast-000069-origin-of-optical-uv-emission-and-late-time-radio-outflows-in-tidal-disruption-events | Origin of Optical/UV Emission and Late-Time Radio Outflows in Tidal Disruption Events | Does the bright optical/UV blackbody emission (T ~ 1-3 x 10^4 K, R ~ 10^14-10^15 cm) in stellar tidal disruption events arise from shock dissipation at self-intersecting debris streams during circularization or from reprocessing of inner X-ray accretion radiation by an optically thick super-Eddington wind envelope, and... | Does the bright optical/UV blackbody emission (T ~ 1-3 x 10^4 K, R ~ 10^14-10^15 cm) in stellar tidal disruption events arise from shock dissipation at self-intersecting debris streams during circularization or from reprocessing of inner X-ray accretion radiation by an optically thick super-Eddington wind envelope, and... | Does the bright optical/UV blackbody emission (T ~ 1-3 x 10^4 K, R ~ 10^14-10^15 cm) in stellar tidal disruption events arise from shock dissipation at self-intersecting debris streams during circularization or from reprocessing of inner X-ray accretion radiation by an optically thick super-Eddington wind envelope, and... | transients_gravitational_waves_multimessenger | 9 | Transients, Gravitational Waves, and Multi-Messenger Astronomy | tidal_disruption_events_and_nuclear_transients | [] | mechanism | [
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UAST-000070 | UAST-000070 | uast-000070-origin-of-the-pair-instability-mass-gap-population-60-120-m-sun-in-binary-black-hole | Origin of the Pair-Instability Mass Gap Population (60-120 M_sun) in Binary Black Hole Mergers | How do binary black hole components with masses inside the theoretical pair-instability supernova mass gap (60 <= M_BH/M_sun <= 120, such as GW190521) form—via hierarchical second-generation black hole mergers in dense star clusters or AGN disks, stellar mergers in young clusters, or downward revision of the 12C(alpha,... | How do binary black hole components with masses inside the theoretical pair-instability supernova mass gap (60 <= M_BH/M_sun <= 120, such as GW190521) form—via hierarchical second-generation black hole mergers in dense star clusters or AGN disks, stellar mergers in young clusters, or downward revision of the 12C(alpha,... | How do binary black hole components with masses inside the theoretical pair-instability supernova mass gap (60 <= M_BH/M_sun <= 120, such as GW190521) form—via hierarchical second-generation black hole mergers in dense star clusters or AGN disks, stellar mergers in young clusters, or downward revision of the 12C(alpha,... | transients_gravitational_waves_multimessenger | 9 | Transients, Gravitational Waves, and Multi-Messenger Astronomy | gravitational_wave_sources_and_populations | [] | origin | [
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] | [
"Gravitational-wave strain waveforms h(t), chirp masses M_c, effective spins chi_eff, and PTA Hellings-Downs spatial correlations",
"Millisecond radio burst dynamic spectra I(nu, t), polarization angle swings, dispersion measures DM, and scintillation timescales",
"Multi-band transient light curves, nebular/pho... | [
"Compact binary formation channels (isolated binary evolution vs dynamical cluster/AGN assembly)",
"Fast radio burst emission radius (magnetosphere vs relativistic shock) and progenitor repetition rate",
"R-process lanthanide mass fraction M_ej, v_ej in kilonovae and debris circularization efficiency in TDEs"
] | [
"Gravitational-wave detector horizon volume scaling (~M_c^15/6) favoring high-mass mergers",
"Fluence threshold and dispersion smearing against high-DM or broad-pulse fast radio bursts"
] | [
"Numerical relativity waveform higher-multipole and eccentric-orbit modeling systematics",
"Host-galaxy vs Milky Way halo dispersion measure partitioning along FRB sightlines"
] | [
"Eccentric dynamical capture vs spin-precessing quasi-circular inspiral in short GW signals",
"Magnetar central engine spin-down vs circumstellar shock interaction in superluminous supernovae"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Transients, Gravitational Waves, and Multi-Messenger Astronomy community syntheses as of 2026-10-16. | multimessenger | decade_scale | Discriminating Baseline astrophysical mechanism in gravitational wave sources and populati from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Gravitational-wave strain waveforms h(t), chirp masses M_c, effective spins chi_. | Current observations from LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110 constrain Compact binary formation channels (isolated binary evolution vs dynamical cluster/AGN, but systematic uncertainties in Numerical relativity waveform higher-multipole and eccentric-orbit mod prevent a definitive resolution. | [
"Baseline astrophysical mechanism in gravitational wave sources and populations constrained by LIGO-Virgo-KAGRA, CHIME/FRB",
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] | [
"High-significance multi-wavelength or dynamical measurement of Gravitational-wave strain waveforms h(t), chirp masses M_c, effective spins chi_eff, and P using LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110.",
"Breaking the model degeneracy between Eccentric dynamical capture vs spin-precessing quasi-circular inspiral in ... | Resolving this question in Transients, Gravitational Waves, and Multi-Messenger Astronomy is essential for calibrating Compact binary formation channels (isolated binary evolution vs dynamical cluste and testing fundamental astrophysical theory. | Time-domain astrophysics, gravitational-wave data analysis and source astrophysics, coherent radiative processes in magnetars/FRBs, and relativistic blast-wave hydrodynamics. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000006",
"support_type": "direct_open_question",
"locator": "Section 2.3: Stellar-Mass Binary Black Hole Populations and Mass Gaps, p. 22",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-022811",
"citation": "Banerjee (2022, Astronomy & Astrophysics)",
... | [
"UAST-000011",
"UAST-023931",
"UAST-018657",
"UAST-017879"
] | null | [] | [
"transients_gravitational_waves_multimessenger",
"gravitational_wave_sources_and_populations",
"pair_instability_mass_gap",
"GW190521",
"hierarchical_mergers",
"nuclear_reaction_rates"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000006). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000071 | UAST-000071 | uast-000071-electromagnetic-counterparts-and-agn-disk-flares-from-binary-black-hole-mergers | Electromagnetic Counterparts and AGN Disk Flares from Binary Black Hole Mergers | Can stellar-mass binary black hole mergers embedded in dense active galactic nucleus accretion disks produce detectable, reproducible optical, UV, or X-ray shock-breakout flares driven by Bondi-Hoyle accretion and gravitational-wave recoil kicks, and how can real counterparts be distinguished from stochastic intrinsic ... | Can stellar-mass binary black hole mergers embedded in dense active galactic nucleus accretion disks produce detectable, reproducible optical, UV, or X-ray shock-breakout flares driven by Bondi-Hoyle accretion and gravitational-wave recoil kicks, and how can real counterparts be distinguished from stochastic intrinsic ... | Can stellar-mass binary black hole mergers embedded in dense active galactic nucleus accretion disks produce detectable, reproducible optical, UV, or X-ray shock-breakout flares driven by Bondi-Hoyle accretion and gravitational-wave recoil kicks, and how can real counterparts be distinguished from stochastic intrinsic ... | transients_gravitational_waves_multimessenger | 9 | Transients, Gravitational Waves, and Multi-Messenger Astronomy | multimessenger_associations_and_counterparts | [] | detection_or_characterization | [
"transient",
"compact_object",
"agn_quasar"
] | population_level | Astrophysical systems in multimessenger associations and counterparts | [
"au",
"pc"
] | [
{
"name": "time_domain_and_multimessenger_universe",
"redshift_min": 0,
"redshift_max": 6,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.8
}
] | [
"gravitational_wave",
"optical",
"uv",
"x_ray"
] | [
"LIGO-Virgo-KAGRA",
"CHIME/FRB",
"DSA-110",
"ASKAP",
"NANOGrav/EPTA/PPTA/IPTA"
] | [
"Gravitational-wave strain waveforms h(t), chirp masses M_c, effective spins chi_eff, and PTA Hellings-Downs spatial correlations",
"Millisecond radio burst dynamic spectra I(nu, t), polarization angle swings, dispersion measures DM, and scintillation timescales",
"Multi-band transient light curves, nebular/pho... | [
"Compact binary formation channels (isolated binary evolution vs dynamical cluster/AGN assembly)",
"Fast radio burst emission radius (magnetosphere vs relativistic shock) and progenitor repetition rate",
"R-process lanthanide mass fraction M_ej, v_ej in kilonovae and debris circularization efficiency in TDEs"
] | [
"Gravitational-wave detector horizon volume scaling (~M_c^15/6) favoring high-mass mergers",
"Fluence threshold and dispersion smearing against high-DM or broad-pulse fast radio bursts"
] | [
"Numerical relativity waveform higher-multipole and eccentric-orbit modeling systematics",
"Host-galaxy vs Milky Way halo dispersion measure partitioning along FRB sightlines"
] | [
"Eccentric dynamical capture vs spin-precessing quasi-circular inspiral in short GW signals",
"Magnetar central engine spin-down vs circumstellar shock interaction in superluminous supernovae"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Transients, Gravitational Waves, and Multi-Messenger Astronomy community syntheses as of 2026-10-16. | multimessenger | decade_scale | Discriminating Baseline astrophysical mechanism in multimessenger associations and counter from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Gravitational-wave strain waveforms h(t), chirp masses M_c, effective spins chi_. | Current observations from LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110 constrain Compact binary formation channels (isolated binary evolution vs dynamical cluster/AGN, but systematic uncertainties in Numerical relativity waveform higher-multipole and eccentric-orbit mod prevent a definitive resolution. | [
"Baseline astrophysical mechanism in multimessenger associations and counterparts constrained by LIGO-Virgo-KAGRA, CHIME/FRB",
"Alternative non-equilibrium, feedback, or multi-component physical model for Electromagnetic Counterparts and AGN Disk Flares from Binary Black Hol"
] | [
"High-significance multi-wavelength or dynamical measurement of Gravitational-wave strain waveforms h(t), chirp masses M_c, effective spins chi_eff, and P using LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110.",
"Breaking the model degeneracy between Eccentric dynamical capture vs spin-precessing quasi-circular inspiral in ... | Resolving this question in Transients, Gravitational Waves, and Multi-Messenger Astronomy is essential for calibrating Compact binary formation channels (isolated binary evolution vs dynamical cluste and testing fundamental astrophysical theory. | Time-domain astrophysics, gravitational-wave data analysis and source astrophysics, coherent radiative processes in magnetars/FRBs, and relativistic blast-wave hydrodynamics. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Appendix D: Multi-Messenger Counterparts to Gravitational Wave Events, p. D-16",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-022081",
"citation": "He et al. (2026, arXiv (astro-ph.HE))",
... | [
"UAST-000011",
"UAST-023201",
"UAST-018149",
"UAST-018785"
] | null | [] | [
"transients_gravitational_waves_multimessenger",
"multimessenger_associations_and_counterparts",
"BBH_counterparts",
"AGN_disk_mergers",
"recoil_kicks",
"multimessenger"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000072 | UAST-000072 | uast-000072-origin-of-the-positron-fraction-excess-above-10-gev-nearby-pulsars-vs-dark-matter-ann | Origin of the Positron Fraction Excess Above 10 GeV: Nearby Pulsars vs Dark Matter Annihilation | Is the rise in the cosmic-ray positron fraction e+ / (e- + e+) between 10 and 300 GeV (and its rollover near ~300-500 GeV measured by PAMELA, AMS-02, and DAMPE) fully accounted for by pair cascades from nearby middle-aged pulsars and their TeV gamma-ray halos (such as Geminga and Monogem), or does it require secondary ... | Is the rise in the cosmic-ray positron fraction e+ / (e- + e+) between 10 and 300 GeV (and its rollover near ~300-500 GeV measured by PAMELA, AMS-02, and DAMPE) fully accounted for by pair cascades from nearby middle-aged pulsars and their TeV gamma-ray halos (such as Geminga and Monogem), or does it require secondary ... | Is the rise in the cosmic-ray positron fraction e+ / (e- + e+) between 10 and 300 GeV (and its rollover near ~300-500 GeV measured by PAMELA, AMS-02, and DAMPE) fully accounted for by pair cascades from nearby middle-aged pulsars and their TeV gamma-ray halos (such as Geminga and Monogem), or does it require secondary ... | cosmic_rays_neutrinos_nonthermal | 10 | Cosmic Rays, Neutrinos, and the Nonthermal Universe | galactic_cosmic_rays_and_pevatrons | [] | model_discrimination | [
"nonthermal_particle",
"compact_object",
"dark_sector"
] | population_level | Astrophysical systems in galactic cosmic rays and pevatrons | [
"pc",
"kpc"
] | [
{
"name": "nonthermal_and_high_energy_universe",
"redshift_min": 0,
"redshift_max": 4,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.2
}
] | [
"cosmic_ray",
"gamma_ray"
] | [
"Pierre Auger Observatory",
"Telescope Array",
"IceCube",
"KM3NeT",
"LHAASO"
] | [
"Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_max>, and arrival direction multipoles",
"High-energy astrophysical neutrino flavor ratios, energy spectrum E^-gamma, and directional point-source excesses",
"GeV-PeV gamma-ray spectra, extended pulsar halo morphologies, and secondar... | [
"Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission fractions",
"Galactic and extragalactic magnetic field deflection angles and cosmic-ray diffusion coefficient D(E)",
"Coronal optical depth tau_gamma_gamma and proton-to-electron power ratio in AGN neutrino cores"
] | [
"Greisen-Zatsepin-Kuzmin (GZK) and photo-disintegration horizon limiting UHECR sources above 50 EeV to < 100 Mpc",
"Earth absorption at PeV-EeV neutrino energies and atmospheric muon/neutrino background cuts"
] | [
"Hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) in air-shower X_max mass inference",
"Galactic interstellar gas column density and diffuse gamma-ray foreground modeling"
] | [
"Intrinsic source spectral cutoff vs propagation photo-disintegration in the UHECR ankle/suppression region",
"Inverse-Compton leptonic emission vs neutral-pion decay hadronic gamma-ray emission"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Cosmic Rays, Neutrinos, and the Nonthermal Universe community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in galactic cosmic rays and pevatrons cons from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_ma. | Current observations from Pierre Auger Observatory, Telescope Array, IceCube constrain Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission fracti, but systematic uncertainties in Hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) in prevent a definitive resolution. | [
"Baseline astrophysical mechanism in galactic cosmic rays and pevatrons constrained by Pierre Auger Observatory, Telescope Array",
"Alternative non-equilibrium, feedback, or multi-component physical model for Origin of the Positron Fraction Excess Above 10 GeV: Nearby Pulsars vs"
] | [
"High-significance multi-wavelength or dynamical measurement of Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_max>, and ar using Pierre Auger Observatory, Telescope Array, IceCube.",
"Breaking the model degeneracy between Intrinsic source spectral cutoff vs propagation photo-disint... | Resolving this question in Cosmic Rays, Neutrinos, and the Nonthermal Universe is essential for calibrating Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission f and testing fundamental astrophysical theory. | High-energy particle astrophysics, diffusive shock acceleration and relativistic magnetic reconnection, cosmic-ray propagation and magnetohydrodynamic turbulence, and multimessenger neutrino/gamma-ray radiative transfer. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000009",
"support_type": "direct_open_question",
"locator": "Section 4.3: Cosmic-Ray Leptons and TeV Halos, p. 46",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-019898",
"citation": "Grimani (2021, arXiv (astro-ph.HE))",
"support_type": "explicit_op... | [
"UAST-000013",
"UAST-021290",
"UAST-003310",
"UAST-006800"
] | null | [] | [
"cosmic_rays_neutrinos_nonthermal",
"galactic_cosmic_rays_and_pevatrons",
"positron_excess",
"AMS_02",
"TeV_halos",
"Geminga"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000009). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000073 | UAST-000073 | uast-000073-anisotropy-and-source-class-of-ultra-high-energy-cosmic-rays-above-8-eev | Anisotropy and Source Class of Ultra-High-Energy Cosmic Rays Above 8 EeV | Which specific extragalactic source class—starburst galaxies, radio-loud active galactic nuclei (such as Centaurus A), tidal disruption events, or magnetar flares—produces the large-scale dipole anisotropy above 8 EeV and intermediate-scale hot spots above 32 EeV observed by the Pierre Auger Observatory and Telescope A... | Which specific extragalactic source class—starburst galaxies, radio-loud active galactic nuclei (such as Centaurus A), tidal disruption events, or magnetar flares—produces the large-scale dipole anisotropy above 8 EeV and intermediate-scale hot spots above 32 EeV observed by the Pierre Auger Observatory and Telescope A... | Which specific extragalactic source class—starburst galaxies, radio-loud active galactic nuclei (such as Centaurus A), tidal disruption events, or magnetar flares—produces the large-scale dipole anisotropy above 8 EeV and intermediate-scale hot spots above 32 EeV observed by the Pierre Auger Observatory and Telescope A... | cosmic_rays_neutrinos_nonthermal | 10 | Cosmic Rays, Neutrinos, and the Nonthermal Universe | ultra_high_energy_cosmic_rays | [] | origin | [
"nonthermal_particle",
"agn_quasar",
"galaxy"
] | population_level | Astrophysical systems in ultra high energy cosmic rays | [
"mpc",
"10_to_100_mpc"
] | [
{
"name": "nonthermal_and_high_energy_universe",
"redshift_min": 0,
"redshift_max": 4,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.2
}
] | [
"cosmic_ray",
"gamma_ray",
"neutrino"
] | [
"Pierre Auger Observatory",
"Telescope Array",
"IceCube",
"KM3NeT",
"LHAASO"
] | [
"Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_max>, and arrival direction multipoles",
"High-energy astrophysical neutrino flavor ratios, energy spectrum E^-gamma, and directional point-source excesses",
"GeV-PeV gamma-ray spectra, extended pulsar halo morphologies, and secondar... | [
"Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission fractions",
"Galactic and extragalactic magnetic field deflection angles and cosmic-ray diffusion coefficient D(E)",
"Coronal optical depth tau_gamma_gamma and proton-to-electron power ratio in AGN neutrino cores"
] | [
"Greisen-Zatsepin-Kuzmin (GZK) and photo-disintegration horizon limiting UHECR sources above 50 EeV to < 100 Mpc",
"Earth absorption at PeV-EeV neutrino energies and atmospheric muon/neutrino background cuts"
] | [
"Hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) in air-shower X_max mass inference",
"Galactic interstellar gas column density and diffuse gamma-ray foreground modeling"
] | [
"Intrinsic source spectral cutoff vs propagation photo-disintegration in the UHECR ankle/suppression region",
"Inverse-Compton leptonic emission vs neutral-pion decay hadronic gamma-ray emission"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Cosmic Rays, Neutrinos, and the Nonthermal Universe community syntheses as of 2026-10-16. | multimessenger | decade_scale | Discriminating Baseline astrophysical mechanism in ultra high energy cosmic rays constrain from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_ma. | Current observations from Pierre Auger Observatory, Telescope Array, IceCube constrain Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission fracti, but systematic uncertainties in Hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) in prevent a definitive resolution. | [
"Baseline astrophysical mechanism in ultra high energy cosmic rays constrained by Pierre Auger Observatory, Telescope Array",
"Alternative non-equilibrium, feedback, or multi-component physical model for Anisotropy and Source Class of Ultra-High-Energy Cosmic Rays Above 8 E"
] | [
"High-significance multi-wavelength or dynamical measurement of Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_max>, and ar using Pierre Auger Observatory, Telescope Array, IceCube.",
"Breaking the model degeneracy between Intrinsic source spectral cutoff vs propagation photo-disint... | Resolving this question in Cosmic Rays, Neutrinos, and the Nonthermal Universe is essential for calibrating Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission f and testing fundamental astrophysical theory. | High-energy particle astrophysics, diffusive shock acceleration and relativistic magnetic reconnection, cosmic-ray propagation and magnetohydrodynamic turbulence, and multimessenger neutrino/gamma-ray radiative transfer. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Appendix D: High-Energy Particles and Cosmic Rays, p. D-19",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-025117",
"citation": "Almeida et al. (2021, International Conference on Rebooting Comp... | [
"UAST-000013",
"UAST-026069",
"UAST-025610",
"UAST-013561"
] | null | [] | [
"cosmic_rays_neutrinos_nonthermal",
"ultra_high_energy_cosmic_rays",
"UHECR_anisotropy",
"Pierre_Auger",
"Telescope_Array",
"starburst_galaxies",
"Centaurus_A"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000074 | UAST-000074 | uast-000074-hadronic-corona-mechanism-in-x-ray-bright-gamma-ray-obscured-neutrino-seyfert-cores-n | Hadronic Corona Mechanism in X-Ray Bright, Gamma-Ray Obscured Neutrino Seyfert Cores (NGC 1068) | What magnetohydrodynamic or shock acceleration process within 10-30 gravitational radii of the supermassive black hole in Seyfert galaxies such as NGC 1068 accelerates protons to 10-100 TeV to produce the observed IceCube neutrino flux while dense X-ray coronal photons absorb the co-produced GeV-TeV gamma rays via gamm... | What magnetohydrodynamic or shock acceleration process within 10-30 gravitational radii of the supermassive black hole in Seyfert galaxies such as NGC 1068 accelerates protons to 10-100 TeV to produce the observed IceCube neutrino flux while dense X-ray coronal photons absorb the co-produced GeV-TeV gamma rays via gamm... | What magnetohydrodynamic or shock acceleration process within 10-30 gravitational radii of the supermassive black hole in Seyfert galaxies such as NGC 1068 accelerates protons to 10-100 TeV to produce the observed IceCube neutrino flux while dense X-ray coronal photons absorb the co-produced GeV-TeV gamma rays via gamm... | cosmic_rays_neutrinos_nonthermal | 10 | Cosmic Rays, Neutrinos, and the Nonthermal Universe | astrophysical_neutrinos | [] | mechanism | [
"agn_quasar",
"nonthermal_particle",
"compact_object"
] | population_level | Astrophysical systems in astrophysical neutrinos | [
"au"
] | [
{
"name": "nonthermal_and_high_energy_universe",
"redshift_min": 0,
"redshift_max": 4,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 12.2
}
] | [
"neutrino",
"x_ray",
"gamma_ray",
"mm_submm"
] | [
"Pierre Auger Observatory",
"Telescope Array",
"IceCube",
"KM3NeT",
"LHAASO"
] | [
"Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_max>, and arrival direction multipoles",
"High-energy astrophysical neutrino flavor ratios, energy spectrum E^-gamma, and directional point-source excesses",
"GeV-PeV gamma-ray spectra, extended pulsar halo morphologies, and secondar... | [
"Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission fractions",
"Galactic and extragalactic magnetic field deflection angles and cosmic-ray diffusion coefficient D(E)",
"Coronal optical depth tau_gamma_gamma and proton-to-electron power ratio in AGN neutrino cores"
] | [
"Greisen-Zatsepin-Kuzmin (GZK) and photo-disintegration horizon limiting UHECR sources above 50 EeV to < 100 Mpc",
"Earth absorption at PeV-EeV neutrino energies and atmospheric muon/neutrino background cuts"
] | [
"Hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) in air-shower X_max mass inference",
"Galactic interstellar gas column density and diffuse gamma-ray foreground modeling"
] | [
"Intrinsic source spectral cutoff vs propagation photo-disintegration in the UHECR ankle/suppression region",
"Inverse-Compton leptonic emission vs neutral-pion decay hadronic gamma-ray emission"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Cosmic Rays, Neutrinos, and the Nonthermal Universe community syntheses as of 2026-10-16. | multimessenger | decade_scale | Discriminating Baseline astrophysical mechanism in astrophysical neutrinos constrained by from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_ma. | Current observations from Pierre Auger Observatory, Telescope Array, IceCube constrain Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission fracti, but systematic uncertainties in Hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) in prevent a definitive resolution. | [
"Baseline astrophysical mechanism in astrophysical neutrinos constrained by Pierre Auger Observatory, Telescope Array",
"Alternative non-equilibrium, feedback, or multi-component physical model for Hadronic Corona Mechanism in X-Ray Bright, Gamma-Ray Obscured Neutrino"
] | [
"High-significance multi-wavelength or dynamical measurement of Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_max>, and ar using Pierre Auger Observatory, Telescope Array, IceCube.",
"Breaking the model degeneracy between Intrinsic source spectral cutoff vs propagation photo-disint... | Resolving this question in Cosmic Rays, Neutrinos, and the Nonthermal Universe is essential for calibrating Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission f and testing fundamental astrophysical theory. | High-energy particle astrophysics, diffusive shock acceleration and relativistic magnetic reconnection, cosmic-ray propagation and magnetohydrodynamic turbulence, and multimessenger neutrino/gamma-ray radiative transfer. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000009",
"support_type": "direct_open_question",
"locator": "Section 5.2: Multimessenger Neutrino and Gamma-Ray Sources, p. 55",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-024852",
"citation": "Fiorillo et al. (2023, The Astrophysical Journal Letters,... | [
"UAST-000013",
"UAST-025804",
"UAST-025501",
"UAST-026126"
] | null | [] | [
"cosmic_rays_neutrinos_nonthermal",
"astrophysical_neutrinos",
"NGC_1068",
"AGN_corona",
"hadronic_acceleration",
"IceCube",
"gamma_ray_obscuration"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000009). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000075 | UAST-000075 | uast-000075-millisecond-pulsar-population-vs-dark-matter-annihilation-origin-of-the-galactic-cent | Millisecond Pulsar Population vs Dark Matter Annihilation Origin of the Galactic Center GeV Excess | Does the spatially extended, spherically symmetric 1-3 GeV gamma-ray excess in the inner few degrees of the Galactic Center observed by Fermi-LAT arise from an unresolved bulge population of thousands of millisecond pulsars (characterized by non-Poissonian photon-count statistics) or from weakly interacting massive par... | Does the spatially extended, spherically symmetric 1-3 GeV gamma-ray excess in the inner few degrees of the Galactic Center observed by Fermi-LAT arise from an unresolved bulge population of thousands of millisecond pulsars (characterized by non-Poissonian photon-count statistics) or from weakly interacting massive par... | Does the spatially extended, spherically symmetric 1-3 GeV gamma-ray excess in the inner few degrees of the Galactic Center observed by Fermi-LAT arise from an unresolved bulge population of thousands of millisecond pulsars (characterized by non-Poissonian photon-count statistics) or from weakly interacting massive par... | cosmic_rays_neutrinos_nonthermal | 10 | Cosmic Rays, Neutrinos, and the Nonthermal Universe | gamma_ray_astronomy_and_gev_tev_sources | [] | model_discrimination | [
"milky_way_component",
"compact_object",
"dark_sector",
"nonthermal_particle"
] | population_level | Astrophysical systems in gamma ray astronomy and gev tev sources | [
"pc",
"kpc"
] | [
{
"name": "nonthermal_and_high_energy_universe",
"redshift_min": 0,
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Cosmic Rays, Neutrinos, and the Nonthermal Universe community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in gamma ray astronomy and gev tev sources from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_ma. | Current observations from Pierre Auger Observatory, Telescope Array, IceCube constrain Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission fracti, but systematic uncertainties in Hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) in prevent a definitive resolution. | [
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{
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{
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"citation": "Eckner et al. (2025, arXiv (astro-ph.HE))",
... | [
"UAST-000013",
"UAST-025567",
"UAST-013582",
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] | null | [] | [
"cosmic_rays_neutrinos_nonthermal",
"gamma_ray_astronomy_and_gev_tev_sources",
"Galactic_Center_GeV_excess",
"Fermi_LAT",
"millisecond_pulsars",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000009). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000076 | UAST-000076 | uast-000076-cosmic-ray-self-confinement-vs-extrinsic-turbulence-and-the-origin-of-the-tev-halo-di | Cosmic-Ray Self-Confinement vs Extrinsic Turbulence and the Origin of the TeV Halo Diffusion Suppression | Why is the cosmic-ray electron/positron diffusion coefficient inside 10-50 pc TeV gamma-ray halos around middle-aged pulsars suppressed by two to three orders of magnitude relative to the average Galactic ISM diffusion coefficient, and is this suppression driven by streaming-instability self-confinement or pre-existing... | Why is the cosmic-ray electron/positron diffusion coefficient inside 10-50 pc TeV gamma-ray halos around middle-aged pulsars suppressed by two to three orders of magnitude relative to the average Galactic ISM diffusion coefficient, and is this suppression driven by streaming-instability self-confinement or pre-existing... | Why is the cosmic-ray electron/positron diffusion coefficient inside 10-50 pc TeV gamma-ray halos around middle-aged pulsars suppressed by two to three orders of magnitude relative to the average Galactic ISM diffusion coefficient, and is this suppression driven by streaming-instability self-confinement or pre-existing... | cosmic_rays_neutrinos_nonthermal | 10 | Cosmic Rays, Neutrinos, and the Nonthermal Universe | particle_acceleration_and_transport | [] | mechanism | [
"nonthermal_particle",
"interstellar_medium",
"compact_object"
] | population_level | Astrophysical systems in particle acceleration and transport | [
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{
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] | [
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"Intrinsic source spectral cutoff vs propagation photo-disintegration in the UHECR ankle/suppression region",
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Cosmic Rays, Neutrinos, and the Nonthermal Universe community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in particle acceleration and transport con from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_ma. | Current observations from Pierre Auger Observatory, Telescope Array, IceCube constrain Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission fracti, but systematic uncertainties in Hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) in prevent a definitive resolution. | [
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{
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{
"source_id": "SRC-AST-005918",
"citation": "Timon et al. (2023, Mon.Not.Roy.Astron.Soc.)",
"support_type": "... | [
"UAST-000013",
"UAST-008674",
"UAST-026023",
"UAST-015361"
] | null | [] | [
"cosmic_rays_neutrinos_nonthermal",
"particle_acceleration_and_transport",
"cosmic_ray_diffusion",
"TeV_halos",
"streaming_instability",
"MHD_turbulence"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000009). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000077 | UAST-000077 | uast-000077-diffuse-galactic-plane-neutrino-emission-diffuse-cosmic-ray-sea-vs-unresolved-hadroni | Diffuse Galactic Plane Neutrino Emission: Diffuse Cosmic-Ray Sea vs Unresolved Hadronic PeVatrons | What fraction of the diffuse TeV-PeV neutrino emission from the Galactic plane detected by IceCube arises from cosmic-ray sea interactions with interstellar molecular gas (pi^0 decay counterpart) versus an unresolved population of compact hadronic PeVatrons (supernova remnants, pulsar-powered sources, or microquasars)? | What fraction of the diffuse TeV-PeV neutrino emission from the Galactic plane detected by IceCube arises from cosmic-ray sea interactions with interstellar molecular gas (pi^0 decay counterpart) versus an unresolved population of compact hadronic PeVatrons (supernova remnants, pulsar-powered sources, or microquasars)? | What fraction of the diffuse TeV-PeV neutrino emission from the Galactic plane detected by IceCube arises from cosmic-ray sea interactions with interstellar molecular gas (pi^0 decay counterpart) versus an unresolved population of compact hadronic PeVatrons (supernova remnants, pulsar-powered sources, or microquasars)?... | cosmic_rays_neutrinos_nonthermal | 10 | Cosmic Rays, Neutrinos, and the Nonthermal Universe | astrophysical_neutrinos | [] | model_discrimination | [
"milky_way_component",
"nonthermal_particle",
"interstellar_medium"
] | population_level | Astrophysical systems in astrophysical neutrinos | [
"pc",
"kpc"
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{
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] | [
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"Intrinsic source spectral cutoff vs propagation photo-disintegration in the UHECR ankle/suppression region",
"Inverse-Compton leptonic emission vs neutral-pion decay hadronic gamma-ray emission"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Cosmic Rays, Neutrinos, and the Nonthermal Universe community syntheses as of 2026-10-16. | multimessenger | decade_scale | Discriminating Baseline astrophysical mechanism in astrophysical neutrinos constrained by from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_ma. | Current observations from Pierre Auger Observatory, Telescope Array, IceCube constrain Maximum particle acceleration rigidity R_max and hadronic vs leptonic emission fracti, but systematic uncertainties in Hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) in prevent a definitive resolution. | [
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] | [
"High-significance multi-wavelength or dynamical measurement of Ultra-high-energy cosmic-ray energy spectrum J(E), depth of shower maximum <X_max>, and ar using Pierre Auger Observatory, Telescope Array, IceCube.",
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{
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"locator": "Appendix D: Neutrino Astronomy, p. D-18",
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{
"source_id": "SRC-AST-024507",
"citation": "Ouyang et al. (2026, arXiv (astro-ph.HE))",
"support_type": "explicit_open_gap_... | [
"UAST-000013",
"UAST-025459",
"UAST-013797",
"UAST-015970"
] | null | [] | [
"cosmic_rays_neutrinos_nonthermal",
"astrophysical_neutrinos",
"Galactic_plane_neutrinos",
"IceCube",
"LHAASO",
"hadronic_PeVatrons"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000078 | UAST-000078 | uast-000078-origin-of-protoplanetary-disk-rings-and-gaps-embedded-protoplanets-vs-magneto-thermal | Origin of Protoplanetary Disk Rings and Gaps: Embedded Protoplanets vs Magneto-Thermal and Ice-Line Instabilities | Are the concentric dust rings, gaps, and spiral arms observed in young (< 1-3 Myr) protoplanetary disks by ALMA universally carved by already-formed Saturn-to-Jupiter-mass protoplanets, or can secular gravitational instability, zonal flows from non-ideal MHD, or dust sintering at volatile snowlines produce rings prior ... | Are the concentric dust rings, gaps, and spiral arms observed in young (< 1-3 Myr) protoplanetary disks by ALMA universally carved by already-formed Saturn-to-Jupiter-mass protoplanets, or can secular gravitational instability, zonal flows from non-ideal MHD, or dust sintering at volatile snowlines produce rings prior ... | Are the concentric dust rings, gaps, and spiral arms observed in young (< 1-3 Myr) protoplanetary disks by ALMA universally carved by already-formed Saturn-to-Jupiter-mass protoplanets, or can secular gravitational instability, zonal flows from non-ideal MHD, or dust sintering at volatile snowlines produce rings prior ... | exoplanets_planetary_system_formation | 11 | Exoplanets and Planetary-System Formation | protoplanetary_disks_and_planet_formation | [] | model_discrimination | [
"protoplanetary_disk",
"exoplanet",
"dust_and_ice"
] | population_level | Astrophysical systems in protoplanetary disks and planet formation | [
"au"
] | [
{
"name": "protoplanetary_disks_to_mature_systems",
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"redshift_max": 0.01,
"lookback_time_gyr_min": 0,
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}
] | [
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"JWST",
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"Kepler",
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"Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, and orbital phase curves",
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"ALMA millimeter dust continuum rings/gaps, polarized scattering, and CO channel-map v... | [
"Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation of state",
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"Protoplanetary disk turbulence parameter alpha, dust-to-gas ratio, and embedded p... | [
"Geometric transit probability (~R_*/a) and RV semi-amplitude bias strongly favoring close-in planets",
"Stellar activity jitter and rotational modulation masking low-mass temperate planet RV signals"
] | [
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"Volatile-rich H2O ocean/ice layer vs silicate core + H2/He envelope in sub-Neptune mass-radius diagrams"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Exoplanets and Planetary-System Formation community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in protoplanetary disks and planet formati from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, . | Current observations from JWST, ALMA, TESS constrain Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation o, but systematic uncertainties in Transit light-source effect (unocculted starspots/faculae) contaminati prevent a definitive resolution. | [
"Baseline astrophysical mechanism in protoplanetary disks and planet formation constrained by JWST, ALMA",
"Alternative non-equilibrium, feedback, or multi-component physical model for Origin of Protoplanetary Disk Rings and Gaps: Embedded Protoplanets vs"
] | [
"High-significance multi-wavelength or dynamical measurement of Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, and orbita using JWST, ALMA, TESS.",
"Breaking the model degeneracy between High-altitude photochemical haze/cloud deck vs high mean-molecular-weight atmosphere in fl to ... | Resolving this question in Exoplanets and Planetary-System Formation is essential for calibrating Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equat and testing fundamental astrophysical theory. | Exoplanet detection and characterization, planetary atmospheric radiative-convective transfer and chemistry, interior structure equations of state, and protoplanetary disk gas-dust hydrodynamics. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Section 2.1: Pathways to Habitable Worlds & Planet Formation, p. 2-11",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-027253",
"citation": "Wu et al. (2023, arXiv (astro-ph.EP))",
"support_... | [
"UAST-000014",
"UAST-027897",
"UAST-028471",
"UAST-028308"
] | null | [] | [
"exoplanets_planetary_system_formation",
"protoplanetary_disks_and_planet_formation",
"protoplanetary_disks",
"ALMA_rings",
"kinematic_kinks",
"snowlines"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000079 | UAST-000079 | uast-000079-origin-of-the-hot-neptune-desert-and-orbital-migration-pathways-of-close-in-giant-pla | Origin of the Hot-Neptune Desert and Orbital Migration Pathways of Close-In Giant Planets | Why is there a stark dearth of short-period (P < 3-4 days) intermediate-mass exoplanets in the 'Neptune desert' (R_p ~ 2-8 R_oplus), and what is the quantitative balance between high-eccentricity tidal migration and tidally disrupted / photoevaporatively stripped envelopes in sculpting this boundary? | Why is there a stark dearth of short-period (P < 3-4 days) intermediate-mass exoplanets in the 'Neptune desert' (R_p ~ 2-8 R_oplus), and what is the quantitative balance between high-eccentricity tidal migration and tidally disrupted / photoevaporatively stripped envelopes in sculpting this boundary? | Why is there a stark dearth of short-period (P < 3-4 days) intermediate-mass exoplanets in the 'Neptune desert' (R_p ~ 2-8 R_oplus), and what is the quantitative balance between high-eccentricity tidal migration and tidally disrupted / photoevaporatively stripped envelopes in sculpting this boundary? Highlighted as a k... | exoplanets_planetary_system_formation | 11 | Exoplanets and Planetary-System Formation | exoplanet_demographics_and_architectures | [] | mechanism | [
"exoplanet",
"star"
] | population_level | Astrophysical systems in exoplanet demographics and architectures | [
"1000km_to_rsun",
"au"
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{
"name": "protoplanetary_disks_to_mature_systems",
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"ALMA millimeter dust continuum rings/gaps, polarized scattering, and CO channel-map v... | [
"Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation of state",
"Atmospheric elemental abundance ratios (C/O, N/O, metallicity [M/H]), vertical temperature profile T(P), and aerosol deck pressure",
"Protoplanetary disk turbulence parameter alpha, dust-to-gas ratio, and embedded p... | [
"Geometric transit probability (~R_*/a) and RV semi-amplitude bias strongly favoring close-in planets",
"Stellar activity jitter and rotational modulation masking low-mass temperate planet RV signals"
] | [
"Transit light-source effect (unocculted starspots/faculae) contaminating transmission spectra around M dwarfs",
"3D day-night terminator limb asymmetries and molecular line-list opacity uncertainties"
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"High-altitude photochemical haze/cloud deck vs high mean-molecular-weight atmosphere in flat transmission spectra",
"Volatile-rich H2O ocean/ice layer vs silicate core + H2/He envelope in sub-Neptune mass-radius diagrams"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Exoplanets and Planetary-System Formation community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in exoplanet demographics and architecture from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, . | Current observations from JWST, ALMA, TESS constrain Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation o, but systematic uncertainties in Transit light-source effect (unocculted starspots/faculae) contaminati prevent a definitive resolution. | [
"Baseline astrophysical mechanism in exoplanet demographics and architectures constrained by JWST, ALMA",
"Alternative non-equilibrium, feedback, or multi-component physical model for Origin of the Hot-Neptune Desert and Orbital Migration Pathways of Clo"
] | [
"High-significance multi-wavelength or dynamical measurement of Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, and orbita using JWST, ALMA, TESS.",
"Breaking the model degeneracy between High-altitude photochemical haze/cloud deck vs high mean-molecular-weight atmosphere in fl to ... | Resolving this question in Exoplanets and Planetary-System Formation is essential for calibrating Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equat and testing fundamental astrophysical theory. | Exoplanet detection and characterization, planetary atmospheric radiative-convective transfer and chemistry, interior structure equations of state, and protoplanetary disk gas-dust hydrodynamics. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000013",
"support_type": "direct_open_question",
"locator": "Section 2.2: Exoplanet Demographics and Evolution, p. 24",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-019347",
"citation": "Eyles-Ferris et al. (2025, Mon Not R Astron Soc (2026))",
"sup... | [
"UAST-000014",
"UAST-020739",
"UAST-018325",
"UAST-030065"
] | null | [] | [
"exoplanets_planetary_system_formation",
"exoplanet_demographics_and_architectures",
"Neptune_desert",
"high_eccentricity_migration",
"atmospheric_stripping",
"hot_Jupiters"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000013). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000080 | UAST-000080 | uast-000080-atmospheric-c-o-ratio-and-metallicity-calibration-of-giant-planet-formation-locations | Atmospheric C/O Ratio and Metallicity Calibration of Giant Planet Formation Locations Relative to Snowlines | Can atmospheric carbon-to-oxygen (C/O), nitrogen-to-oxygen (N/O), and refractory-to-volatile abundance ratios measured via JWST and high-resolution ground-based spectroscopy uniquely reconstruct where a gas giant formed relative to disk H2O, CO2, and CO snowlines, or do chemical disk evolution and planetesimal/pebble p... | Can atmospheric carbon-to-oxygen (C/O), nitrogen-to-oxygen (N/O), and refractory-to-volatile abundance ratios measured via JWST and high-resolution ground-based spectroscopy uniquely reconstruct where a gas giant formed relative to disk H2O, CO2, and CO snowlines, or do chemical disk evolution and planetesimal/pebble p... | Can atmospheric carbon-to-oxygen (C/O), nitrogen-to-oxygen (N/O), and refractory-to-volatile abundance ratios measured via JWST and high-resolution ground-based spectroscopy uniquely reconstruct where a gas giant formed relative to disk H2O, CO2, and CO snowlines, or do chemical disk evolution and planetesimal/pebble p... | exoplanets_planetary_system_formation | 11 | Exoplanets and Planetary-System Formation | exoplanet_atmospheres_and_climates | [] | model_discrimination | [
"exoplanet",
"protoplanetary_disk"
] | population_level | Astrophysical systems in exoplanet atmospheres and climates | [
"1000km_to_rsun",
"au"
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"Protoplanetary disk turbulence parameter alpha, dust-to-gas ratio, and embedded p... | [
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Exoplanets and Planetary-System Formation community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in exoplanet atmospheres and climates cons from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, . | Current observations from JWST, ALMA, TESS constrain Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation o, but systematic uncertainties in Transit light-source effect (unocculted starspots/faculae) contaminati prevent a definitive resolution. | [
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{
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"locator": "Appendix F: Exoplanets, Astrobiology, and the Solar System, p. F-8",
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},
{
"source_id": "SRC-AST-029606",
"citation": "Team et al. (2026, arXiv (astro-ph.EP))",
"support_t... | [
"UAST-000014",
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"UAST-028116",
"UAST-027459"
] | null | [] | [
"exoplanets_planetary_system_formation",
"exoplanet_atmospheres_and_climates",
"C_to_O_ratio",
"exoplanet_atmospheres",
"snowlines",
"JWST_spectroscopy"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000081 | UAST-000081 | uast-000081-compositional-degeneracy-and-interior-state-of-sub-neptunes-hycean-water-worlds-vs-mi | Compositional Degeneracy and Interior State of Sub-Neptunes: 'Hycean' Water Worlds vs Miscible Magma-Ocean Envelope Worlds | For temperate and warm sub-Neptunes (1.7 <= R_p/R_oplus <= 3.0) with bulk densities consistent with both volatile-rich water worlds and rocky cores topped by H2/He envelopes, does chemical equilibration between a deep silicate magma ocean and a hydrogen envelope (producing endogenous H2O, SiO, and CH4/CO2 depletion) mi... | For temperate and warm sub-Neptunes (1.7 <= R_p/R_oplus <= 3.0) with bulk densities consistent with both volatile-rich water worlds and rocky cores topped by H2/He envelopes, does chemical equilibration between a deep silicate magma ocean and a hydrogen envelope (producing endogenous H2O, SiO, and CH4/CO2 depletion) mi... | For temperate and warm sub-Neptunes (1.7 <= R_p/R_oplus <= 3.0) with bulk densities consistent with both volatile-rich water worlds and rocky cores topped by H2/He envelopes, does chemical equilibration between a deep silicate magma ocean and a hydrogen envelope (producing endogenous H2O, SiO, and CH4/CO2 depletion) mi... | exoplanets_planetary_system_formation | 11 | Exoplanets and Planetary-System Formation | exoplanet_interiors_and_bulk_composition | [] | model_discrimination | [
"exoplanet"
] | population_level | Astrophysical systems in exoplanet interiors and bulk composition | [
"km_to_1000km",
"1000km_to_rsun"
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"ALMA millimeter dust continuum rings/gaps, polarized scattering, and CO channel-map v... | [
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"Geometric transit probability (~R_*/a) and RV semi-amplitude bias strongly favoring close-in planets",
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"Transit light-source effect (unocculted starspots/faculae) contaminating transmission spectra around M dwarfs",
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Exoplanets and Planetary-System Formation community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in exoplanet interiors and bulk compositio from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, . | Current observations from JWST, ALMA, TESS constrain Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation o, but systematic uncertainties in Transit light-source effect (unocculted starspots/faculae) contaminati prevent a definitive resolution. | [
"Baseline astrophysical mechanism in exoplanet interiors and bulk composition constrained by JWST, ALMA",
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] | [
"High-significance multi-wavelength or dynamical measurement of Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, and orbita using JWST, ALMA, TESS.",
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{
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{
"source_id": "SRC-AST-029607",
"citation": "Tang et al. (2026, arXiv (astro-ph.EP))",
"support_type": "ex... | [
"UAST-000014",
"UAST-030048",
"UAST-027222",
"UAST-027428"
] | null | [] | [
"exoplanets_planetary_system_formation",
"exoplanet_interiors_and_bulk_composition",
"sub_Neptunes",
"Hycean_worlds",
"magma_ocean",
"compositional_degeneracy"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000013). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000082 | UAST-000082 | uast-000082-core-mantle-differentiation-and-volatile-fractions-of-exo-planetesimals-accreted-by-p | Core-Mantle Differentiation and Volatile Fractions of Exo-Planetesimals Accreted by Polluted White Dwarfs | What do heavy-element photospheric abundances (Fe, Ni, Mg, Si, Ca, O, C, S) in externally polluted white dwarfs reveal about the frequency of iron-core differentiation, water retention, and carbon depletion in rocky planetesimals across extrasolar planetary systems? | What do heavy-element photospheric abundances (Fe, Ni, Mg, Si, Ca, O, C, S) in externally polluted white dwarfs reveal about the frequency of iron-core differentiation, water retention, and carbon depletion in rocky planetesimals across extrasolar planetary systems? | What do heavy-element photospheric abundances (Fe, Ni, Mg, Si, Ca, O, C, S) in externally polluted white dwarfs reveal about the frequency of iron-core differentiation, water retention, and carbon depletion in rocky planetesimals across extrasolar planetary systems? Highlighted as a key community research question in P... | exoplanets_planetary_system_formation | 11 | Exoplanets and Planetary-System Formation | debris_disks_polluted_white_dwarfs_and_exocomets | [] | detection_or_characterization | [
"compact_object",
"exoplanet",
"solar_system_body"
] | population_level | Astrophysical systems in debris disks polluted white dwarfs and exocomets | [
"km_to_1000km",
"au"
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{
"name": "protoplanetary_disks_to_mature_systems",
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"lookback_time_gyr_min": 0,
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"ALMA millimeter dust continuum rings/gaps, polarized scattering, and CO channel-map v... | [
"Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation of state",
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"Geometric transit probability (~R_*/a) and RV semi-amplitude bias strongly favoring close-in planets",
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Exoplanets and Planetary-System Formation community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in debris disks polluted white dwarfs and from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, . | Current observations from JWST, ALMA, TESS constrain Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation o, but systematic uncertainties in Transit light-source effect (unocculted starspots/faculae) contaminati prevent a definitive resolution. | [
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] | [
"High-significance multi-wavelength or dynamical measurement of Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, and orbita using JWST, ALMA, TESS.",
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{
"source_id": "SRC-AST-000001",
"support_type": "direct_open_question",
"locator": "Appendix F: Planetary System Remnants and White Dwarf Pollution, p. F-12",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-028892",
"citation": "Klein et al. (2009, Astrophysics & Astronomy Liter... | [
"UAST-000014",
"UAST-029536",
"UAST-032926",
"UAST-031423"
] | null | [] | [
"exoplanets_planetary_system_formation",
"debris_disks_polluted_white_dwarfs_and_exocomets",
"polluted_white_dwarfs",
"exoplanetesimals",
"core_mantle_differentiation",
"debris_disks"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000083 | UAST-000083 | uast-000083-turbulent-viscosity-alpha-vs-magnetocentrifugal-disk-winds-driving-protoplanetary-dis | Turbulent Viscosity alpha vs Magnetocentrifugal Disk Winds Driving Protoplanetary Disk Accretion | Is angular momentum transport in the planet-forming regions (1-50 AU) of protoplanetary disks driven primarily by magnetorotational instability turbulence (with effective viscosity alpha ~ 10^-3 to 10^-2) or by laminar non-ideal MHD magnetocentrifugal disk winds in weakly ionized 'dead zones' where turbulent velocities... | Is angular momentum transport in the planet-forming regions (1-50 AU) of protoplanetary disks driven primarily by magnetorotational instability turbulence (with effective viscosity alpha ~ 10^-3 to 10^-2) or by laminar non-ideal MHD magnetocentrifugal disk winds in weakly ionized 'dead zones' where turbulent velocities... | Is angular momentum transport in the planet-forming regions (1-50 AU) of protoplanetary disks driven primarily by magnetorotational instability turbulence (with effective viscosity alpha ~ 10^-3 to 10^-2) or by laminar non-ideal MHD magnetocentrifugal disk winds in weakly ionized 'dead zones' where turbulent velocities... | exoplanets_planetary_system_formation | 11 | Exoplanets and Planetary-System Formation | protoplanetary_disks_and_planet_formation | [] | model_discrimination | [
"protoplanetary_disk"
] | population_level | Astrophysical systems in protoplanetary disks and planet formation | [
"au"
] | [
{
"name": "protoplanetary_disks_to_mature_systems",
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"redshift_max": 0.01,
"lookback_time_gyr_min": 0,
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}
] | [
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"Kepler",
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"ALMA millimeter dust continuum rings/gaps, polarized scattering, and CO channel-map v... | [
"Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation of state",
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"Protoplanetary disk turbulence parameter alpha, dust-to-gas ratio, and embedded p... | [
"Geometric transit probability (~R_*/a) and RV semi-amplitude bias strongly favoring close-in planets",
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Exoplanets and Planetary-System Formation community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in protoplanetary disks and planet formati from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Transit depth spectrum (R_p/R_*)^2(lambda), secondary eclipse thermal emission, . | Current observations from JWST, ALMA, TESS constrain Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equation o, but systematic uncertainties in Transit light-source effect (unocculted starspots/faculae) contaminati prevent a definitive resolution. | [
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"Breaking the model degeneracy between High-altitude photochemical haze/cloud deck vs high mean-molecular-weight atmosphere in fl to ... | Resolving this question in Exoplanets and Planetary-System Formation is essential for calibrating Planetary bulk density rho_p, core-to-envelope mass fraction, and interior equat and testing fundamental astrophysical theory. | Exoplanet detection and characterization, planetary atmospheric radiative-convective transfer and chemistry, interior structure equations of state, and protoplanetary disk gas-dust hydrodynamics. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000008",
"support_type": "direct_open_question",
"locator": "Section 3.4: Protoplanetary Disk Evolution and Winds, p. 38",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-032446",
"citation": "Lesur et al. (2014, arXiv (astro-ph.SR))",
"support_type": ... | [
"UAST-000014",
"UAST-032720",
"UAST-021165",
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"exoplanets_planetary_system_formation",
"protoplanetary_disks_and_planet_formation",
"protoplanetary_disks",
"MHD_disk_winds",
"magnetorotational_instability",
"dead_zones"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000008). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000084 | UAST-000084 | uast-000084-origin-of-the-dilute-compositionally-graded-cores-in-jupiter-and-saturn | Origin of the Dilute, Compositionally Graded Cores in Jupiter and Saturn | Was Jupiter's and Saturn's radially extended 'dilute' or 'fuzzy' heavy-element core (extending to ~30-60% of the planetary radius as revealed by Juno gravity harmonics and Cassini ring seismology) formed by a giant embryo head-on impact, convective double-diffusive mixing, or gradual heavy-element enrichment during run... | Was Jupiter's and Saturn's radially extended 'dilute' or 'fuzzy' heavy-element core (extending to ~30-60% of the planetary radius as revealed by Juno gravity harmonics and Cassini ring seismology) formed by a giant embryo head-on impact, convective double-diffusive mixing, or gradual heavy-element enrichment during run... | Was Jupiter's and Saturn's radially extended 'dilute' or 'fuzzy' heavy-element core (extending to ~30-60% of the planetary radius as revealed by Juno gravity harmonics and Cassini ring seismology) formed by a giant embryo head-on impact, convective double-diffusive mixing, or gradual heavy-element enrichment during run... | solar_system_worlds_small_bodies | 12 | Solar-System Worlds and Small Bodies | giant_planets_and_ice_giants | [] | origin | [
"solar_system_body"
] | population_level | Astrophysical systems in giant planets and ice giants | [
"km_to_1000km",
"1000km_to_rsun"
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{
"name": "solar_nebula_to_present_solar_system",
"redshift_min": 0,
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] | [
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"JUICE",
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"Deep wide-field astrometric orbits of trans-Neptunian obje... | [
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] | [
"Internal radial density profile vs deep zonal wind flow depth in giant planet gravity harmonics",
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Solar-System Worlds and Small Bodies community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in giant planets and ice giants constraine from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Spacecraft Doppler gravity harmonics J_2n, tidal Love numbers k_2/h_2, and magne. | Current observations from Juno, Europa Clipper, JUICE constrain Giant planet core mass distribution, heavy-element radial gradient, and H-He phase se, but systematic uncertainties in High-pressure hydrogen-helium-water equation of state and electrical c prevent a definitive resolution. | [
"Baseline astrophysical mechanism in giant planets and ice giants constrained by Juno, Europa Clipper",
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] | [
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"Breaking the model degeneracy between Internal radial density profile vs deep zonal wind flow depth in giant planet gravi... | Resolving this question in Solar-System Worlds and Small Bodies is essential for calibrating Giant planet core mass distribution, heavy-element radial gradient, and H-He pha and testing fundamental astrophysical theory. | Planetary geophysics and interior structure, cosmochemistry and meteoritics, orbital dynamics and celestial mechanics, and icy moon oceanography. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
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"locator": "Section 4: Origins — Giant Planet Interiors and Formation, p. 4-15",
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{
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"supp... | [
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000010). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000085 | UAST-000085 | uast-000085-timing-and-atmospheric-loss-mechanisms-of-early-martian-liquid-water-and-carbonate-re | Timing and Atmospheric Loss Mechanisms of Early Martian Liquid Water and Carbonate Reservoirs | How did early Mars (3.5-4.1 Gyr ago) sustain episodic or persistent surface liquid water under a faint young Sun, and what fraction of its primordial CO2 and H2O inventory was sequestered into crustal carbonates and hydrated minerals versus lost to space via solar-wind sputtering and photochemical escape? | How did early Mars (3.5-4.1 Gyr ago) sustain episodic or persistent surface liquid water under a faint young Sun, and what fraction of its primordial CO2 and H2O inventory was sequestered into crustal carbonates and hydrated minerals versus lost to space via solar-wind sputtering and photochemical escape? | How did early Mars (3.5-4.1 Gyr ago) sustain episodic or persistent surface liquid water under a faint young Sun, and what fraction of its primordial CO2 and H2O inventory was sequestered into crustal carbonates and hydrated minerals versus lost to space via solar-wind sputtering and photochemical escape? Highlighted a... | solar_system_worlds_small_bodies | 12 | Solar-System Worlds and Small Bodies | terrestrial_planets_and_The_Moon | [] | mechanism | [
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000010). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000086 | UAST-000086 | uast-000086-tidal-dissipation-mechanics-and-seafloor-hydrothermal-activity-in-europa-and-enceladu | Tidal Dissipation Mechanics and Seafloor Hydrothermal Activity in Europa and Enceladus | Where is tidal mechanical energy primarily dissipated in ocean worlds such as Europa and Enceladus—within the viscoelastic convecting ice shell, by turbulent dissipation in the subsurface liquid ocean, or within a porous, serpentinizing rocky core—and can this dissipation sustain long-lived hydrothermal activity over 4... | Where is tidal mechanical energy primarily dissipated in ocean worlds such as Europa and Enceladus—within the viscoelastic convecting ice shell, by turbulent dissipation in the subsurface liquid ocean, or within a porous, serpentinizing rocky core—and can this dissipation sustain long-lived hydrothermal activity over 4... | Where is tidal mechanical energy primarily dissipated in ocean worlds such as Europa and Enceladus—within the viscoelastic convecting ice shell, by turbulent dissipation in the subsurface liquid ocean, or within a porous, serpentinizing rocky core—and can this dissipation sustain long-lived hydrothermal activity over 4... | solar_system_worlds_small_bodies | 12 | Solar-System Worlds and Small Bodies | ocean_worlds_and_icy_moons | [] | mechanism | [
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{
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"citation": "Shoji et al. (2016, A&A 599, L10 (2017))",
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"UAST-000015",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000010). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000087 | UAST-000087 | uast-000087-origin-of-the-carbonaceous-vs-non-carbonaceous-nc-cc-meteorite-isotopic-dichotomy-in | Origin of the Carbonaceous vs Non-Carbonaceous (NC-CC) Meteorite Isotopic Dichotomy in the Early Solar Nebula | What physical barrier in the proto-solar nebula—early growth of proto-Jupiter's gap, a pressure bump near the water snowline, or two distinct infall episodes from the parental molecular cloud—maintained the nucleosynthetic isotopic separation between non-carbonaceous (inner Solar System) and carbonaceous (outer Solar S... | What physical barrier in the proto-solar nebula—early growth of proto-Jupiter's gap, a pressure bump near the water snowline, or two distinct infall episodes from the parental molecular cloud—maintained the nucleosynthetic isotopic separation between non-carbonaceous (inner Solar System) and carbonaceous (outer Solar S... | What physical barrier in the proto-solar nebula—early growth of proto-Jupiter's gap, a pressure bump near the water snowline, or two distinct infall episodes from the parental molecular cloud—maintained the nucleosynthetic isotopic separation between non-carbonaceous (inner Solar System) and carbonaceous (outer Solar S... | solar_system_worlds_small_bodies | 12 | Solar-System Worlds and Small Bodies | asteroids_comets_and_meteoritics | [] | origin | [
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... | [
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000010). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000088 | UAST-000088 | uast-000088-dynamical-origin-of-high-perihelion-sednoids-and-extreme-trans-neptunian-object-orbit | Dynamical Origin of High-Perihelion Sednoids and Extreme Trans-Neptunian Object Orbital Clustering | Were the detached, high-perihelion orbits of Sedna, 2012 VP113, and 541132 Leleākūhonua (q > 45-80 AU, a > 250 AU) emplaced by a distant perturbing planet (5-10 M_oplus at 300-800 AU), by stellar flybys in the Sun's natal birth cluster, or by secular inclination instability of a massive primordial planetesimal disk? | Were the detached, high-perihelion orbits of Sedna, 2012 VP113, and 541132 Leleākūhonua (q > 45-80 AU, a > 250 AU) emplaced by a distant perturbing planet (5-10 M_oplus at 300-800 AU), by stellar flybys in the Sun's natal birth cluster, or by secular inclination instability of a massive primordial planetesimal disk? | Were the detached, high-perihelion orbits of Sedna, 2012 VP113, and 541132 Leleākūhonua (q > 45-80 AU, a > 250 AU) emplaced by a distant perturbing planet (5-10 M_oplus at 300-800 AU), by stellar flybys in the Sun's natal birth cluster, or by secular inclination instability of a massive primordial planetesimal disk? Hi... | solar_system_worlds_small_bodies | 12 | Solar-System Worlds and Small Bodies | trans_neptunian_objects_kuiper_belt_and_oort_cloud | [] | model_discrimination | [
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] | population_level | Astrophysical systems in trans neptunian objects kuiper belt and oort cloud | [
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{
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{
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000010). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000089 | UAST-000089 | uast-000089-production-rate-and-ejection-mechanisms-of-1i-oumuamua-like-volatile-depleted-vs-2i-b | Production Rate and Ejection Mechanisms of 1I/'Oumuamua-Like Volatile-Depleted vs 2I/Borisov-Like Interstellar Objects | What planetary-system dynamical ejection mechanisms account for the high local number density (~0.1-0.2 AU^-3) of interstellar objects and the stark compositional contrast between hyper-volatile-driven, dust-poor 1I/'Oumuamua and CO-rich cometary 2I/Borisov? | What planetary-system dynamical ejection mechanisms account for the high local number density (~0.1-0.2 AU^-3) of interstellar objects and the stark compositional contrast between hyper-volatile-driven, dust-poor 1I/'Oumuamua and CO-rich cometary 2I/Borisov? | What planetary-system dynamical ejection mechanisms account for the high local number density (~0.1-0.2 AU^-3) of interstellar objects and the stark compositional contrast between hyper-volatile-driven, dust-poor 1I/'Oumuamua and CO-rich cometary 2I/Borisov? Highlighted as a key community research question in Science w... | solar_system_worlds_small_bodies | 12 | Solar-System Worlds and Small Bodies | interstellar_objects_and_solar_system_dynamics | [] | origin | [
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"Alternative non-equilibrium, feedback, or multi-component physical model for Production Rate and Ejection Mechanisms of 1I/'Oumuamua-Like Volatile-"
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UAST-000092 | UAST-000092 | uast-000092-simultaneous-detection-of-o2-o3-and-ch4-chemical-disequilibrium-vs-photochemical-fals | Simultaneous Detection of O2/O3 and CH4 Chemical Disequilibrium vs Photochemical False Positives in Direct-Imaging Spectra | What spectral resolution, wavelength coverage (0.2-2.0 um), and signal-to-noise ratio are required for a future Habitable Worlds Observatory coronagraphic mission to detect coexisting O2/O3, H2O, and CH4 thermodynamic disequilibrium in an Earth-twin atmosphere while ruling out abiotic O2 accumulation from H2O/CO2 photo... | What spectral resolution, wavelength coverage (0.2-2.0 um), and signal-to-noise ratio are required for a future Habitable Worlds Observatory coronagraphic mission to detect coexisting O2/O3, H2O, and CH4 thermodynamic disequilibrium in an Earth-twin atmosphere while ruling out abiotic O2 accumulation from H2O/CO2 photo... | What spectral resolution, wavelength coverage (0.2-2.0 um), and signal-to-noise ratio are required for a future Habitable Worlds Observatory coronagraphic mission to detect coexisting O2/O3, H2O, and CH4 thermodynamic disequilibrium in an Earth-twin atmosphere while ruling out abiotic O2 accumulation from H2O/CO2 photo... | astrobiology_habitability_biosignatures_technosignatures | 13 | Astrobiology, Habitability, Biosignatures, and Technosignatures | exoplanet_biosignatures_and_false_positives | [] | detection_or_characterization | [
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{
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000093 | UAST-000093 | uast-000093-biotic-vs-serpentinization-abiotic-origin-of-organic-macromolecules-and-phosphates-in | Biotic vs Serpentinization/Abiotic Origin of Organic Macromolecules and Phosphates in Enceladus Plume Ice Grains | Can mass-spectrometric analysis of Enceladus plume ice grains (measuring amino acid enantiomeric excess, lipid chain-length periodicity, and C/N/H isotopic fractionation) definitively distinguish prebiotic hydrothermal synthesis associated with olivine serpentinization from extant methanogenic or chemolithoautotrophic ... | Can mass-spectrometric analysis of Enceladus plume ice grains (measuring amino acid enantiomeric excess, lipid chain-length periodicity, and C/N/H isotopic fractionation) definitively distinguish prebiotic hydrothermal synthesis associated with olivine serpentinization from extant methanogenic or chemolithoautotrophic ... | Can mass-spectrometric analysis of Enceladus plume ice grains (measuring amino acid enantiomeric excess, lipid chain-length periodicity, and C/N/H isotopic fractionation) definitively distinguish prebiotic hydrothermal synthesis associated with olivine serpentinization from extant methanogenic or chemolithoautotrophic ... | astrobiology_habitability_biosignatures_technosignatures | 13 | Astrobiology, Habitability, Biosignatures, and Technosignatures | solar_system_biosignatures_and_life_detection | [] | model_discrimination | [
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{
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000010). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000094 | UAST-000094 | uast-000094-upper-limits-on-narrowband-radio-optical-laser-and-waste-heat-infrared-technosignatur | Upper Limits on Narrowband Radio, Optical Laser, and Waste-Heat Infrared Technosignatures in the Local Galactic Volume | What fraction of stars within 100 pc and galaxies in the Local Universe host persistent narrowband (< 10 Hz) radio transmitters, nanosecond optical/NIR laser pulses, or anomalous mid-infrared waste heat (Dyson-swarm-like infrared excesses) above natural astrophysical dust backgrounds? | What fraction of stars within 100 pc and galaxies in the Local Universe host persistent narrowband (< 10 Hz) radio transmitters, nanosecond optical/NIR laser pulses, or anomalous mid-infrared waste heat (Dyson-swarm-like infrared excesses) above natural astrophysical dust backgrounds? | What fraction of stars within 100 pc and galaxies in the Local Universe host persistent narrowband (< 10 Hz) radio transmitters, nanosecond optical/NIR laser pulses, or anomalous mid-infrared waste heat (Dyson-swarm-like infrared excesses) above natural astrophysical dust backgrounds? Highlighted as a key community res... | astrobiology_habitability_biosignatures_technosignatures | 13 | Astrobiology, Habitability, Biosignatures, and Technosignatures | technosignatures_and_seti | [] | value_or_bound | [
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{
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"locator": "Section 5.4: Technosignatures and SETI in the Context of Astrobiology, p. 115",
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{
"source_id": "SRC-AST-025418",
"citation": "James et al. (2017, EPJ Web Conf., Volume 135... | [
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"astrobiology_habitability_biosignatures_technosignatures",
"technosignatures_and_seti",
"technosignatures",
"SETI",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000012). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000095 | UAST-000095 | uast-000095-ultraviolet-prebiotic-threshold-vs-atmospheric-photolysis-hazard-around-low-mass-star | Ultraviolet Prebiotic Threshold vs Atmospheric Photolysis Hazard Around Low-Mass Stars | Do quiescent low-mass M dwarfs provide sufficient near-ultraviolet (200-280 nm) photon flux to drive cyanosulfidic prebiotic ribonucleotide synthesis on rocky planet surfaces without relying on frequent superflares that simultaneously erode the atmosphere via extreme-UV hydrodynamic escape? | Do quiescent low-mass M dwarfs provide sufficient near-ultraviolet (200-280 nm) photon flux to drive cyanosulfidic prebiotic ribonucleotide synthesis on rocky planet surfaces without relying on frequent superflares that simultaneously erode the atmosphere via extreme-UV hydrodynamic escape? | Do quiescent low-mass M dwarfs provide sufficient near-ultraviolet (200-280 nm) photon flux to drive cyanosulfidic prebiotic ribonucleotide synthesis on rocky planet surfaces without relying on frequent superflares that simultaneously erode the atmosphere via extreme-UV hydrodynamic escape? Highlighted as a key communi... | astrobiology_habitability_biosignatures_technosignatures | 13 | Astrobiology, Habitability, Biosignatures, and Technosignatures | circumstellar_and_galactic_habitability | [] | tension_resolution | [
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"star"
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{
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{
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"citation": "Ranjan et al. (2017, Ranjan, S., Wordsworth, R., & Sasse... | [
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"astrobiology_habitability_biosignatures_technosignatures",
"circumstellar_and_galactic_habitability",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000012). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000096 | UAST-000096 | uast-000096-the-solar-abundance-problem-spectroscopic-low-metallicity-photosphere-vs-helioseismic | The Solar Abundance Problem: Spectroscopic Low-Metallicity Photosphere vs Helioseismic Sound-Speed Profile | How can the tension between 3D non-LTE solar photospheric chemical abundance determinations (specifically C, N, O, and Ne) and the higher interior metal opacity required by helioseismic sound-speed inversions, convection-zone depth, and Borexino CNO solar neutrino fluxes be fully resolved? | How can the tension between 3D non-LTE solar photospheric chemical abundance determinations (specifically C, N, O, and Ne) and the higher interior metal opacity required by helioseismic sound-speed inversions, convection-zone depth, and Borexino CNO solar neutrino fluxes be fully resolved? | How can the tension between 3D non-LTE solar photospheric chemical abundance determinations (specifically C, N, O, and Ne) and the higher interior metal opacity required by helioseismic sound-speed inversions, convection-zone depth, and Borexino CNO solar neutrino fluxes be fully resolved? Highlighted as a key communit... | solar_stellar_activity_heliospheric | 14 | Solar, Stellar-Activity, and Heliospheric Astronomy | solar_interior_dynamo_and_cycle | [] | tension_resolution | [
"star",
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"Projection foreshortening and Zeeman saturation near the solar limb and polar regions",
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Solar, Stellar-Activity, and Heliospheric Astronomy community syntheses as of 2026-10-16. | multimessenger | decade_scale | Discriminating Baseline astrophysical mechanism in solar interior dynamo and cycle constra from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Full-disk and high-resolution spectropolarimetric vector magnetograms B(x, y, t). | Current observations from Parker Solar Probe, Solar Orbiter, DKIST constrain Coronal heating volumetric dissipation rate Q_heat and reconnection vs wave-turbulenc, but systematic uncertainties in 180-degree azimuth disambiguation and optically thin line-of-sight int prevent a definitive resolution. | [
"Baseline astrophysical mechanism in solar interior dynamo and cycle constrained by Parker Solar Probe, Solar Orbiter",
"Alternative non-equilibrium, feedback, or multi-component physical model for The Solar Abundance Problem: Spectroscopic Low-Metallicity Photosphere"
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{
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{
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"solar_interior_dynamo_and_cycle",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000011). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000097 | UAST-000097 | uast-000097-deep-meridional-circulation-profile-and-polar-field-precursors-of-solar-cycle-amplitu | Deep Meridional Circulation Profile and Polar Field Precursors of Solar Cycle Amplitude | Does the Sun's meridional circulation consist of a single poleward-at-surface, equatorward-at-tachocline cell or radially stacked multi-cell flows, and what nonlinear quenching mechanism governs polar magnetic field buildup and triggers Grand Minima such as the Maunder Minimum? | Does the Sun's meridional circulation consist of a single poleward-at-surface, equatorward-at-tachocline cell or radially stacked multi-cell flows, and what nonlinear quenching mechanism governs polar magnetic field buildup and triggers Grand Minima such as the Maunder Minimum? | Does the Sun's meridional circulation consist of a single poleward-at-surface, equatorward-at-tachocline cell or radially stacked multi-cell flows, and what nonlinear quenching mechanism governs polar magnetic field buildup and triggers Grand Minima such as the Maunder Minimum? Highlighted as a key community research q... | solar_stellar_activity_heliospheric | 14 | Solar, Stellar-Activity, and Heliospheric Astronomy | solar_interior_dynamo_and_cycle | [] | mechanism | [
"star",
"solar_system_body"
] | population_level | Astrophysical systems in solar interior dynamo and cycle | [
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{
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"locator": "Section 2.2: Solar Cycle Predictability and Interior Flows, p. 32",
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{
"source_id": "SRC-AST-034597",
"citation": "Zhao et al. (2013, arXiv (astro-ph.SR))",
"support_ty... | [
"UAST-000017",
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"solar_interior_dynamo_and_cycle",
"solar_dynamo",
"meridional_circulation",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000011). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000098 | UAST-000098 | uast-000098-onset-trigger-of-coronal-mass-ejections-magnetohydrodynamic-torus-kink-instability-vs | Onset Trigger of Coronal Mass Ejections: Magnetohydrodynamic Torus/Kink Instability vs Tether-Cutting/Breakout Reconnection | What observable photospheric and coronal magnetic field parameters determine whether a sheared, twisted solar active region erupts as a fast coronal mass ejection via ideal MHD torus/kink instability or magnetic breakout/tether-cutting reconnection versus remaining a confined flare? | What observable photospheric and coronal magnetic field parameters determine whether a sheared, twisted solar active region erupts as a fast coronal mass ejection via ideal MHD torus/kink instability or magnetic breakout/tether-cutting reconnection versus remaining a confined flare? | What observable photospheric and coronal magnetic field parameters determine whether a sheared, twisted solar active region erupts as a fast coronal mass ejection via ideal MHD torus/kink instability or magnetic breakout/tether-cutting reconnection versus remaining a confined flare? Highlighted as a key community resea... | solar_stellar_activity_heliospheric | 14 | Solar, Stellar-Activity, and Heliospheric Astronomy | solar_flares_cmes_and_magnetic_reconnection | [] | model_discrimination | [
"star",
"solar_system_body"
] | population_level | Astrophysical systems in solar flares cmes and magnetic reconnection | [
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{
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{
"source_id": "SRC-AST-033827",
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] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000011). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000099 | UAST-000099 | uast-000099-electron-acceleration-efficiency-in-solar-flares-how-do-reconnecting-current-sheets-a | Electron Acceleration Efficiency in Solar Flares: How Do Reconnecting Current Sheets Accelerate > 10^36 Electrons/s? | How does magnetic reconnection in a macroscopic solar flare current sheet convert up to 30-50% of the released magnetic energy into non-thermal 10-100 keV electrons (the solar flare 'number problem') without rapid return-current beam instability quenching the acceleration? | How does magnetic reconnection in a macroscopic solar flare current sheet convert up to 30-50% of the released magnetic energy into non-thermal 10-100 keV electrons (the solar flare 'number problem') without rapid return-current beam instability quenching the acceleration? | How does magnetic reconnection in a macroscopic solar flare current sheet convert up to 30-50% of the released magnetic energy into non-thermal 10-100 keV electrons (the solar flare 'number problem') without rapid return-current beam instability quenching the acceleration? Highlighted as a key community research questi... | solar_stellar_activity_heliospheric | 14 | Solar, Stellar-Activity, and Heliospheric Astronomy | solar_flares_cmes_and_magnetic_reconnection | [] | mechanism | [
"star",
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] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Solar, Stellar-Activity, and Heliospheric Astronomy community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in solar flares cmes and magnetic reconnec from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Full-disk and high-resolution spectropolarimetric vector magnetograms B(x, y, t). | Current observations from Parker Solar Probe, Solar Orbiter, DKIST constrain Coronal heating volumetric dissipation rate Q_heat and reconnection vs wave-turbulenc, but systematic uncertainties in 180-degree azimuth disambiguation and optically thin line-of-sight int prevent a definitive resolution. | [
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{
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{
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"number_problem",
"magnetic_islands"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000011). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
UAST-000100 | UAST-000100 | uast-000100-origin-of-parker-solar-probe-magnetic-switchbacks-and-near-sun-alfv-nic-turbulence | Origin of Parker Solar Probe Magnetic 'Switchbacks' and Near-Sun Alfvénic Turbulence | Are the ubiquitous S-shaped magnetic field reversals ('switchbacks') observed by Parker Solar Probe inside 0.3 AU generated at the base of the corona by interchange magnetic reconnection between open and closed loops, or do they grow in-situ during outward expansion of large-amplitude Alfvénic turbulence? | Are the ubiquitous S-shaped magnetic field reversals ('switchbacks') observed by Parker Solar Probe inside 0.3 AU generated at the base of the corona by interchange magnetic reconnection between open and closed loops, or do they grow in-situ during outward expansion of large-amplitude Alfvénic turbulence? | Are the ubiquitous S-shaped magnetic field reversals ('switchbacks') observed by Parker Solar Probe inside 0.3 AU generated at the base of the corona by interchange magnetic reconnection between open and closed loops, or do they grow in-situ during outward expansion of large-amplitude Alfvénic turbulence? Highlighted a... | solar_stellar_activity_heliospheric | 14 | Solar, Stellar-Activity, and Heliospheric Astronomy | solar_wind_turbulence_and_heliosphere | [] | origin | [
"star",
"heliosphere"
] | population_level | Astrophysical systems in solar wind turbulence and heliosphere | [
"km_to_1000km",
"1000km_to_rsun",
"au"
] | [
{
"name": "modern_solar_and_stellar_cycles",
"redshift_min": 0,
"redshift_max": 0.001,
"lookback_time_gyr_min": 0,
"lookback_time_gyr_max": 0.01
}
] | [
"radio_cm_m_lowfreq",
"uv",
"optical"
] | [
"Parker Solar Probe",
"Solar Orbiter",
"DKIST",
"SDO",
"IRIS"
] | [
"Full-disk and high-resolution spectropolarimetric vector magnetograms B(x, y, t) and helioseismic p-mode travel times",
"Extreme-UV and X-ray coronal loop differential emission measures, Doppler velocities, and non-thermal line widths",
"In-situ solar wind proton/alpha/electron velocity distribution functions,... | [
"Coronal heating volumetric dissipation rate Q_heat and reconnection vs wave-turbulence energy flux",
"Interior meridional circulation velocity u_theta(r, theta), tachocline shear, and alpha-Omega dynamo quenching",
"CME initiation instability threshold and particle acceleration efficiency in reconnecting curre... | [
"Projection foreshortening and Zeeman saturation near the solar limb and polar regions",
"Single-spacecraft trajectory sampling along radial heliospheric cuts"
] | [
"180-degree azimuth disambiguation and optically thin line-of-sight integration in coronal magnetometry",
"Non-equilibrium ionization and kappa-distribution departures from local thermodynamic equilibrium in the corona"
] | [
"High-frequency Alfvén wave turbulent dissipation vs unresolved impulsive nanoflare magnetic reconnection",
"Deep interior radiative opacity enhancements vs photospheric 3D non-LTE abundance revisions in the solar abundance problem"
] | open | true | partial_observational_constraint | active_debate | 2026-10-16T00:00:00 | Verified as 'open' across recent peer-reviewed literature and Solar, Stellar-Activity, and Heliospheric Astronomy community syntheses as of 2026-10-16. | observational_and_theoretical | decade_scale | Discriminating Baseline astrophysical mechanism in solar wind turbulence and heliosphere c from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Full-disk and high-resolution spectropolarimetric vector magnetograms B(x, y, t). | Current observations from Parker Solar Probe, Solar Orbiter, DKIST constrain Coronal heating volumetric dissipation rate Q_heat and reconnection vs wave-turbulenc, but systematic uncertainties in 180-degree azimuth disambiguation and optically thin line-of-sight int prevent a definitive resolution. | [
"Baseline astrophysical mechanism in solar wind turbulence and heliosphere constrained by Parker Solar Probe, Solar Orbiter",
"Alternative non-equilibrium, feedback, or multi-component physical model for Origin of Parker Solar Probe Magnetic 'Switchbacks' and Near-Sun Alfvé"
] | [
"High-significance multi-wavelength or dynamical measurement of Full-disk and high-resolution spectropolarimetric vector magnetograms B(x, y, t) and helio using Parker Solar Probe, Solar Orbiter, DKIST.",
"Breaking the model degeneracy between High-frequency Alfvén wave turbulent dissipation vs unresolved impulsi... | Resolving this question in Solar, Stellar-Activity, and Heliospheric Astronomy is essential for calibrating Coronal heating volumetric dissipation rate Q_heat and reconnection vs wave-turb and testing fundamental astrophysical theory. | Solar and stellar magnetohydrodynamics, helioseismology and dynamo theory, magnetic reconnection and kinetic plasma turbulence, and heliospheric space physics. | 4 | Highlighted priority question in major international astronomy decadal survey or agency roadmap. | true | 0 | [
{
"source_id": "SRC-AST-000011",
"support_type": "direct_open_question",
"locator": "Section 2.4: Coronal Heating and the Young Solar Wind, p. 38",
"verbatim_quote_used": false
},
{
"source_id": "SRC-AST-033251",
"citation": "Pandit et al. (2026, arXiv (astro-ph.SR))",
"support_type"... | [
"UAST-000017",
"UAST-033322",
"UAST-034047",
"UAST-033792"
] | null | [] | [
"solar_stellar_activity_heliospheric",
"solar_wind_turbulence_and_heliosphere",
"magnetic_switchbacks",
"Parker_Solar_Probe",
"interchange_reconnection",
"Alfvenic_turbulence"
] | none | Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000011). | 1.1.0 | 2026-10-15T12:00:00 | 2026-10-16T12:00:00 |
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