REVIEW 5 cited by
Radial oscillations of relativistic stars
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
Radial oscillations of relativistic stars
read the original abstract
We present a new survey of the radial oscillation modes of neutron stars. This study complements and corrects earlier studies of radial oscillations. We present an extensive list of frequencies for the most common equations of state and some more recent ones. In order to check the accuracy, we use two different numerical schemes which yield the same results. The stimulation for this work comes from the need of the groups that evolve the full nonlinear Einstein equation to have reliable results from perturbation theory for comparison.
Forward citations
Cited by 5 Pith papers
-
Reaction-constrained composition \(g\)-modes in neutron stars with antikaon condensates, hyperons, and \(\Delta(1232)\) resonances
Antikaon condensates create a distinct composition g-mode that survives fast kaon equilibration, while strong Delta equilibration suppresses the Delta-driven mode except where a frozen Lambda gradient survives.
-
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.
-
Radial Oscillations of Viscous Stars
Viscosity damps neutron-star radial modes on ms timescales, shifts frequencies by up to ~1% at ζ∼10^30 g/cm/s, produces overdamped modes above ∼10^31, and cannot stabilize unstable stars in Eckart or BDNK theory.
-
Neutron stars more compact than black holes in quasi-topological gravity: Equilibrium configurations and radial stability
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.
-
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.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.