Confirmation of 77 new heavily reddened quasars at 1.5 < z < 3.9 with high luminosities and extinctions, showing they are deficient in hot and warm dust relative to blue quasars and supporting a blow-out feedback phase.
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On Massive Neutron Cores
22 Pith papers cite this work, alongside 3,960 external citations. Polarity classification is still indexing.
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Bayesian analysis of a smooth hadron-quark crossover EOS finds current observations tightly constrain the density dependence of nuclear symmetry energy while leaving highest-density hadronic and quark-matter parameters only weakly constrained.
A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
Extends thermal field theory to fermions with angular momentum and shows neutrino production in rotating neutron stars grows indefinitely with angular velocity near the inverse system size.
Derives GR jump conditions and self-similar shock solutions for SIS collapse to BH, showing shocks up to 0.4c, accretion suppressed by factor 5-7, and shock energy release ~10% of enclosed rest mass.
Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
Middle-aged PWNe exhibit diverse reverberation-phase evolution but converge to Sedov-like states; 2D instabilities increase apparent size by up to 50% without changing global dynamics, supporting 1D model robustness.
A semi-supervised VAE trained on Skyrme EOS data reconstructs equations of state with mean absolute percentage errors under 0.14% using two supervised observables (M_max, R_1.4) and one variational latent variable.
Statistical combination of sub-threshold post-merger signals from 50-70 BNS events can constrain the maximum mass of hot neutron stars to 11-20% fractional uncertainty, potentially translating to 12-21% on the cold TOV mass.
Mass-gap compact objects could be hybrid stars only with very early deconfinement and stiff quark matter; confirming 1.4 M⊙ twin stars would cap hybrid-star maximum mass below 2.2 M⊙.
Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.
New effective potentials derived from projections of the Einstein equations approximate GR corrections in Newtonian core-collapse supernova simulations and match full GR results closely.
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
Significant X-ray flux blocking in 4U 1746-37 allows the neutron star to have canonical mass and radius values of 1.59 solar masses and 13 km or 2.12 solar masses and 9.8 km.
Tidal deformability modeling for pulsar companions enables constraints on their equations of state by matching predicted orbital precession to timing data from four systems.
An extended linear sigma model with delta meson and negative sigma_piN produces a symmetry-energy plateau and stiffer EOS that satisfies neutron-star and nuclear constraints.
The (axial-)vector meson extended linear sigma model yields an equation of state for quark matter that satisfies astrophysical constraints on compact star masses and radii.
A double-polytropic EOS family is identified that satisfies multimessenger constraints with M_max around 2.45 solar masses, R_1.4 of 11.3 km, and Lambda_1.4 between 485-512 while remaining causal.
The chapter summarizes established nuclear many-body theory formalisms for calculating low-energy neutrino cross sections in nuclear matter and their implications for astrophysics.
Strong magnetic fields in compact stars induce Landau quantization and magnetic-moment couplings that change the equation of state and allow additional degrees of freedom such as hyperons, Delta resonances, and quark matter.
Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.
citing papers explorer
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Hidden Monsters with SPHEREx I: A goldmine for heavily reddened quasars at cosmic noon
Confirmation of 77 new heavily reddened quasars at 1.5 < z < 3.9 with high luminosities and extinctions, showing they are deficient in hot and warm dust relative to blue quasars and supporting a blow-out feedback phase.
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Bayesian Constraints on the Neutron Star Equation of State with a Smooth Hadron-Quark Crossover
Bayesian analysis of a smooth hadron-quark crossover EOS finds current observations tightly constrain the density dependence of nuclear symmetry energy while leaving highest-density hadronic and quark-matter parameters only weakly constrained.
-
Constrained Gaussian-process bridge prior for neutron-star equation-of-state inference
A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
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Fermion Thermal Field Theory for a Rotating Plasma (with Applications to Neutron Stars)
Extends thermal field theory to fermions with angular momentum and shows neutrino production in rotating neutron stars grows indefinitely with angular velocity near the inverse system size.
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General Relativistic Shock Wave Solutions with Black Hole Formation: The Singular Isothermal Sphere Case
Derives GR jump conditions and self-similar shock solutions for SIS collapse to BH, showing shocks up to 0.4c, accretion suppressed by factor 5-7, and shock energy release ~10% of enclosed rest mass.
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As above, so below: assessing extremeness of the neutron-star equation of state based on the unstable branch
Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
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Modelling the Dynamics of Middle-Aged Pulsar Wind Nebulae in the Reverberation Phase
Middle-aged PWNe exhibit diverse reverberation-phase evolution but converge to Sedov-like states; 2D instabilities increase apparent size by up to 50% without changing global dynamics, supporting 1D model robustness.
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A Semi-Supervised Variational Autoencoder for Generating Neutron Star Equations of State
A semi-supervised VAE trained on Skyrme EOS data reconstructs equations of state with mean absolute percentage errors under 0.14% using two supervised observables (M_max, R_1.4) and one variational latent variable.
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Sub-threshold post-merger gravitational waves can constrain the hot nuclear equation of state
Statistical combination of sub-threshold post-merger signals from 50-70 BNS events can constrain the maximum mass of hot neutron stars to 11-20% fractional uncertainty, potentially translating to 12-21% on the cold TOV mass.
-
Hybrid stars among mass gap objects are excluded by twin stars at $1.4\,M_\odot$
Mass-gap compact objects could be hybrid stars only with very early deconfinement and stiff quark matter; confirming 1.4 M⊙ twin stars would cap hybrid-star maximum mass below 2.2 M⊙.
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Pulse profile modelling of the 2024 outburst of the accreting millisecond pulsar SRGA J144459.2-604207
Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.
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Approximating General Relativity in Core-Collapse Supernova Simulations
New effective potentials derived from projections of the Einstein equations approximate GR corrections in Newtonian core-collapse supernova simulations and match full GR results closely.
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Bayesian analysis of the shear modulus in the neutron-star crust
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
-
The compact neutron star in 4U 1746-37 revisited: Reassessing the mass and radius
Significant X-ray flux blocking in 4U 1746-37 allows the neutron star to have canonical mass and radius values of 1.59 solar masses and 13 km or 2.12 solar masses and 9.8 km.
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What Are Pulsar Companions Made of? Using Gravitational Tides to Probe Their Compositions
Tidal deformability modeling for pulsar companions enables constraints on their equations of state by matching predicted orbital precession to timing data from four systems.
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Nuclear matter properties and neutron star structures from an extended linear sigma model
An extended linear sigma model with delta meson and negative sigma_piN produces a symmetry-energy plateau and stiffer EOS that satisfies neutron-star and nuclear constraints.
-
Compact star properties from an extended linear sigma model
The (axial-)vector meson extended linear sigma model yields an equation of state for quark matter that satisfies astrophysical constraints on compact star masses and radii.
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An Analytical Toy Equation of State for Neutron Stars Consistent with Current Observations
A double-polytropic EOS family is identified that satisfies multimessenger constraints with M_max around 2.45 solar masses, R_1.4 of 11.3 km, and Lambda_1.4 between 485-512 while remaining causal.
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Neutrino Cross Sections: Low Energy
The chapter summarizes established nuclear many-body theory formalisms for calculating low-energy neutrino cross sections in nuclear matter and their implications for astrophysics.
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Dense Matter and Compact Stars in Strong Magnetic Fields
Strong magnetic fields in compact stars induce Landau quantization and magnetic-moment couplings that change the equation of state and allow additional degrees of freedom such as hyperons, Delta resonances, and quark matter.
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Nuclear Physics of Binary Neutron Star Mergers
Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.
- On the Possibility of a Strong First-Order Phase Transition in Neutron Stars