A new relativistic linear perturbation formalism is derived for polar modes in gravitationally coupled two-fluid neutron stars, with numerical computation of representative f- and p-mode spectra classified by dominant fluid character.
Probing the Equation of State of Nuclear Matter via Neutron Star Asteroseismology
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
abstract
We general relativistically calculate the frequency of fundamental torsional oscillations of neutron star crusts, where we focus on the crystalline properties obtained from macroscopic nuclear models in a way depending on the equation of state of nuclear matter. We find that the calculated frequency is sensitive to the density dependence of the symmetry energy, but almost independent of the incompressibility of symmetric nuclear matter. By identifying the lowest-frequency quasi-periodic oscillation in giant flares observed from soft gamma-ray repeaters as the fundamental torsional mode and allowing for the dependence of the calculated frequency on stellar models, we provide a lower limit of the density derivative of the symmetry energy as $L\simeq 50$ MeV.
fields
gr-qc 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
Dark matter admixed neutron stars show up to 12% thinner crusts and higher torsional oscillation frequencies than pure neutron stars when dark matter forms a core, with analytical formulas matching numerics at sub-percent level.
citing papers explorer
-
Non-radial pulsations of gravitationally coupled two-fluid neutron stars in general relativity
A new relativistic linear perturbation formalism is derived for polar modes in gravitationally coupled two-fluid neutron stars, with numerical computation of representative f- and p-mode spectra classified by dominant fluid character.
-
The crust of dark-matter admixed neutron stars: bulk properties and torsional oscillations
Dark matter admixed neutron stars show up to 12% thinner crusts and higher torsional oscillation frequencies than pure neutron stars when dark matter forms a core, with analytical formulas matching numerics at sub-percent level.