Hybrid stars containing the 2SC+<dd> phase cool more slowly than those with the 2SC phase because inherited 3P2 superfluidity suppresses quark beta decay, producing cooling curves close to the CFL case.
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Relativistic Shapiro delay measurements of an extremely massive millisecond pul- sar
13 Pith papers cite this work. Polarity classification is still indexing.
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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.
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.
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.
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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Cooling of Hybrid Stars with a 2SC+$<dd>$ Phase
Hybrid stars containing the 2SC+<dd> phase cool more slowly than those with the 2SC phase because inherited 3P2 superfluidity suppresses quark beta decay, producing cooling curves close to the CFL case.
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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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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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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.
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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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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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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.