Field equation analysis near infinity in massive Hellings-Nordtvedt theory restricts the model to two single-coupling sectors; the A²R sector yields asymptotically flat Schwarzschild black holes with radial vector fields and neutron stars with measurable deviations from GR while satisfying weak-fiel
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A unified equation of state of dense matter and neutron star structure
Mixed citation behavior. Most common role is background (43%).
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43% of classified citations
abstract
An equation of state (EOS) of neutron star matter, describing both the neutron star crust and the liquid core, is calculated. It is based on the effective nuclear interaction SLy of the Skyrme type, which is particularly suitable for the application to the calculation of the properties of very neutron rich matter (Chabanat et al. 1997, 1998). The structure of the crust, and its EOS, is calculated in the T=0 approximation, and under the assumption of the ground state composition. The crust-core transition is a very weakly first-order phase transition, with relative density jump of about one percent. The EOS of the liquid core is calculated assuming (minimal) n-p-e-mu composition. Parameters of static neutron stars are calculated and compared with existing observational data on neutron stars. The minimum and maximum masses of static neutron stars are 0.094 M_sun and 2.05 M_sun, respectively. Effects of rotation on the minimum and the maximum mass of neutron stars are briefly discussed.
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UNVERDICTED 18representative citing papers
Stable neutron-star configurations denser than black holes exist in quasi-topological gravity and may produce detectable gravitational-wave echoes.
Heavy scalar fields in neutron stars form interior shell-localized profiles that reshape the effective equation of state and break the I-Q relation while remaining hidden from binary pulsar observations.
Future high-frequency-sensitive GW detectors can distinguish binary neutron star from low-mass black hole mergers in late phases, enabling separation of merger rates and constraints on heavy non-annihilating dark matter via transmuted black holes.
Bayesian NS EoS study using full nuclear posterior distributions and consistent crust modeling finds increased surface thickness and crustal moment of inertia relative to prior work.
Increasing the bosonic dark matter fraction in admixed neutron stars shifts axial quasi-normal mode frequencies and damping times, can reorder mode hierarchy, and drives a transition from neutron-star-like to boson-star-like ringdown behavior.
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.
Large initial baryon asymmetry allows Hubble patches to collapse into primordial neutron stars arrested by nuclear pressure, requiring later entropy dilution to match observed Y_B and BBN.
In quasi-topological gravity, neutron stars can surpass black-hole compactness with universal high-density behavior and theory corrections that stabilize radially unstable configurations from general relativity.
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.
A small vacuum-like dark-energy admixture in neutron stars with 400 MeV–1 GeV fermionic dark matter shrinks halo-induced radius differences from several kilometers to sub-kilometer scales and mass differences to ≲1%.
Simulations of ET and CE networks show delays degrade localization metrics far more than SNR, with LIGO India greatly reducing the impact for multi-messenger and stochastic searches.
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.
Axial w-mode frequencies of anisotropic neutron stars decrease monotonically with mass, depend approximately linearly on compactness with anisotropy modifying slope and intercept, damping times increase with mass, and empirical expressions are given for both as functions of compactness and anisotrop
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.
Precision timing of PSR J1738+0333 from EPTA and NANOGrav data yields the tightest strong-field constraints on Einstein-aether parameters from any single binary pulsar.
citing papers explorer
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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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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.