Systematic numerical survey classifies four types of slow stable hybrid star branches and shows slow conversion opens new viable parameter space for stiff hadronic models.
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Relativistic Shapiro delay measurements of an extremely massive millisecond pul- sar
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Causality anchored to χEFT at low density implies the closed-form bound R(2.0 M_⊙) ≤ 1.16 R(1.4 M_⊙) − 1.1 km for neutron stars sharing one causal EoS, saturated by an analytic one-parameter family.
Non-parametric EOS construction from crust to pQCD forces a sound-speed peak and softening that realizes a generalized quark-hadron crossover in massive neutron stars.
Mass and radius of PSR J0030+0451 measured as 1.44 solar masses and 13.02 km, improving astrophysical constraints on the cold dense matter equation of state.
Lambda hyperons equilibrate rapidly in post-collapse proto-neutron stars through nonleptonic NN to N Lambda processes and enhance low-energy muon neutrino opacities beyond nucleonic contributions.
Hybrid stars with a 2SC+⟨dd⟩ quark core cool hotter than with 2SC and near CFL; with a 3P2 gap near 5×10^8 K their cooling curves pass through the observed temperatures of 3C58, Vela Jr., and Vela-like pulsars.
A conservative f(R,T) gravity reformulation decouples the gravitational sector from the microphysical equation of state, enabling computation of neutron star mass-radius relations and tidal deformabilities that satisfy current astrophysical constraints.
A physics-informed Bayesian neural network learns neutron-star equations of state from theoretical priors and constraints, then generates posterior mass-radius and mass-tidal-deformability distributions consistent with NICER radii and 2-solar-mass limits.
Hierarchical Bayesian inference on 20 high-SNR simulated binary neutron star events shows a linear lnΛ-lnQ relation suffices and constrains dynamical Chern-Simons gravity length scale to ≤10 km.
A constrained evolutionary pipeline identifies over 14,000 causal EoS reconciling GW170817 and GW190814 with non-monotonic sound speeds, M_max 2.3-2.8 solar masses, and R_1.4 around 12 km.
Roughly half of realistic neutron-star equations of state produce stars with negative Ricci scalar inside, and an improved analytic fit links gravitational mass M to baryonic mass Mb with maximum 3 percent variance.
Hybrid star EOS constructed from QCDSR couplings in RMF hadronic model and bag/NJL quark models with Gibbs/Maxwell transitions yields mass-radius and tidal deformability predictions.
Slow strong hadron-quark phase transitions allow stable hybrid-star branches that accommodate both high-mass and low-radius observations in two viable patterns from a parameter scan.
Moderate positive pressure anisotropy raises neutron star maximum mass to about 2.4 solar masses and compactness by up to 20 percent, with curvature scalars tied to matter showing strong sensitivity while the Weyl scalar stays largely insensitive.
Nonparametric GP-based high-density extensions yield softer EOS posteriors with larger uncertainties than parametric PP extensions when jointly constrained by multi-messenger neutron star observations.
Fisher-matrix forecasts show Cosmic Explorer and Einstein Telescope can probe sub-solar PBHs to z~3 and distinguish PBHs from neutron stars up to z~0.2 via lack of tidal deformability.
A review of spin effects, superfluidity, and magnetic fields in neutron matter and their influence on neutron-star structure, superfluid phases, and rotational dynamics.
citing papers explorer
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Systematic study of the morphology and length of slow stable hybrid star branches
Systematic numerical survey classifies four types of slow stable hybrid star branches and shows slow conversion opens new viable parameter space for stiff hadronic models.
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Causality alone bounds the maximum radius difference between different-mass neutron stars
Causality anchored to χEFT at low density implies the closed-form bound R(2.0 M_⊙) ≤ 1.16 R(1.4 M_⊙) − 1.1 km for neutron stars sharing one causal EoS, saturated by an analytic one-parameter family.
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The Non-parametric Equation of State Realizes a Generalized Quark-Hadron Crossover
Non-parametric EOS construction from crust to pQCD forces a sound-speed peak and softening that realizes a generalized quark-hadron crossover in massive neutron stars.
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PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
Mass and radius of PSR J0030+0451 measured as 1.44 solar masses and 13.02 km, improving astrophysical constraints on the cold dense matter equation of state.
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$\Lambda$ hyperons in core-collapse supernovae: Equilibration and neutrino opacities
Lambda hyperons equilibrate rapidly in post-collapse proto-neutron stars through nonleptonic NN to N Lambda processes and enhance low-energy muon neutrino opacities beyond nucleonic contributions.
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Cooling of Hybrid Stars with a 2SC+$<dd>$ Phase
Hybrid stars with a 2SC+⟨dd⟩ quark core cool hotter than with 2SC and near CFL; with a 3P2 gap near 5×10^8 K their cooling curves pass through the observed temperatures of 3C58, Vela Jr., and Vela-like pulsars.
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Neutron stars in a conservative $f(R,T)$ gravity
A conservative f(R,T) gravity reformulation decouples the gravitational sector from the microphysical equation of state, enabling computation of neutron star mass-radius relations and tidal deformabilities that satisfy current astrophysical constraints.
-
A Physics Informed Bayesian Neural Network for the Neutron Star Equation of State
A physics-informed Bayesian neural network learns neutron-star equations of state from theoretical priors and constraints, then generates posterior mass-radius and mass-tidal-deformability distributions consistent with NICER radii and 2-solar-mass limits.
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Inferring neutron-star Love-Q relations from gravitational waves in the hierarchical Bayesian framework
Hierarchical Bayesian inference on 20 high-SNR simulated binary neutron star events shows a linear lnΛ-lnQ relation suffices and constrains dynamical Chern-Simons gravity length scale to ≤10 km.
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Reconciling GW170817 and GW190814 with a Nonmonotonic Sound-Speed Equation of State
A constrained evolutionary pipeline identifies over 14,000 causal EoS reconciling GW170817 and GW190814 with non-monotonic sound speeds, M_max 2.3-2.8 solar masses, and R_1.4 around 12 km.
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General gravitational properties of neutron stars: curvature invariants, binding energy, and trace anomaly
Roughly half of realistic neutron-star equations of state produce stars with negative Ricci scalar inside, and an improved analytic fit links gravitational mass M to baryonic mass Mb with maximum 3 percent variance.
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Hybrid stars with hyperons: structure based on QCD sum rule coupling constants
Hybrid star EOS constructed from QCDSR couplings in RMF hadronic model and bag/NJL quark models with Gibbs/Maxwell transitions yields mass-radius and tidal deformability predictions.
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Can a Slow and Strong Phase Transition in Neutron Stars Relieve Major Compact-Star Observation Tensions?
Slow strong hadron-quark phase transitions allow stable hybrid-star branches that accommodate both high-mass and low-radius observations in two viable patterns from a parameter scan.
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Impact of Anisotropy on Neutron Star Structure and Curvature
Moderate positive pressure anisotropy raises neutron star maximum mass to about 2.4 solar masses and compactness by up to 20 percent, with curvature scalars tied to matter showing strong sensitivity while the Weyl scalar stays largely insensitive.
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Equation of State Extrapolation Systematics: Parametric vs. Nonparametric Inference of Neutron Star Structure
Nonparametric GP-based high-density extensions yield softer EOS posteriors with larger uncertainties than parametric PP extensions when jointly constrained by multi-messenger neutron star observations.
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Primordial black holes versus their impersonators at gravitational wave observatories
Fisher-matrix forecasts show Cosmic Explorer and Einstein Telescope can probe sub-solar PBHs to z~3 and distinguish PBHs from neutron stars up to z~0.2 via lack of tidal deformability.
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Spin effects in superfluidity, neutron matter and neutron stars
A review of spin effects, superfluidity, and magnetic fields in neutron matter and their influence on neutron-star structure, superfluid phases, and rotational dynamics.