REVIEW 10 cited by
Analytical representations of unified equations of state of neutron-star matter
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Signed reviews
read the original abstract
Analytical representations are derived for two equations of state (EOSs) of neutron-star matter: FPS and SLy. Each of these EOSs is unified, that is, it describes the crust and the core of a neutron star using the same physical model. Two versions of the EOS parametrization are considered. In the first one, pressure and mass density are given as functions of the baryon density. In the second version, pressure, mass density, and baryon density are given as functions of the pseudo-enthalpy, which makes this representation particularly useful for 2-D calculations of stationary rotating configurations of neutron stars.
Forward citations
Cited by 10 Pith papers
-
Black holes and neutron stars in massive Hellings-Nordtvedt theory
In massive Hellings-Nordtvedt theory, a nonzero vector vacuum asymptotically forbids both curvature-vector couplings at once, and the A²R sector yields Schwarzschild-like black holes plus neutron stars that can deviat...
-
Neutron stars more compact than black holes as a probe of strong-field gravity
Stable neutron-star configurations denser than black holes exist in quasi-topological gravity and may produce detectable gravitational-wave echoes.
-
Neutron stars more compact than black holes in quasi-topological gravity: Equilibrium configurations and radial stability
Neutron stars in quasi-topological gravity can be more compact than black holes and radially stable across several equations of state.
-
Neutron stars in degenerate higher-order scalar-tensor theories: Axial perturbations
Axial quasinormal modes of neutron stars in a one-parameter DHOST gravity family deviate from general relativity and obey a Regge-Wheeler-like equation in an effective conformal metric.
-
Neutron star in Logarithmic model of Cartan $F(R)$ gravity
In Cartan F(R) gravity with a logarithmic potential, a scalar field can raise the minimum neutron star mass to near one solar mass, but only for hand-tuned parameters that imply a huge vacuum energy.
-
A Neutron Star Hidden Inside a Black Hole
A two-fluid Tolman-Oppenheimer-Volkoff calculation with Einasto dark matter halos produces static solutions where g_rr^{-1} turns negative in a shell outside the neutron star, which the authors call a neutron star ins...
-
Radial Oscillations of Neutron Stars with Vector-Induced Scalar Hair
In scalar-vector-tensor gravity, the vector-curvature coupling alters neutron star mass-radius curves and radial oscillation frequencies while preserving the coincidence of maximum mass with the onset of radial instability.
-
I-Love-Q relations for Neutron Stars with Dark Energy
I-Love-Q universal relations remain valid within about 1% for neutron stars whose equation of state includes a coupled dark energy fluid in Lambda-CDM and quintessence-like models.
-
Probing up-down quark matter via gravitational waves
Up-down quark stars in the two-families scenario yield tidal deformabilities compatible with GW170817, constraining the effective bag constant to approximately 50 MeV/fm^3.
-
Neutron stars with primary scalar hair
Neutron stars with primary scalar hair in a DHOST subfamily are more compact than GR predictions and develop singularities above a critical scalar charge threshold.
Discussion (0). Continue with ORCID to comment.