The equation of state and radial oscillations of neutron stars
Ting-Ting Sun, Zi-Yue Zheng, Huan Chen, G. Fiorella Burgio, and, Hans-Josef Schulze
TL;DR
This paper studies the radial oscillations of neutron and hybrid stars using advanced equations of state, aiming to connect oscillation frequencies with star stability, maximum mass, and quark matter presence.
Contribution
It introduces a detailed analysis of neutron star oscillations with modern equations of state, linking oscillation eigenfrequencies to star stability and composition.
Findings
Eigenfrequencies determine maximum stable mass of neutron stars.
Radial oscillation frequencies can indicate the presence of quark matter.
Results align with the stability criterion dM/dρ_c=0.
Abstract
We investigate radial oscillations of pure neutron stars and hybrid stars, employing equations of state of nuclear matter from Brueckner-Hartree-Fock theory, and of quark matter from the Dyson-Schwinger quark model, performing a Gibbs construction for the mixed phase in hybrid stars. We calculate the eigenfrequencies and corresponding oscillation functions. Our results for the zero points of the first-order radial oscillation frequencies give the maximum mass of stable neutron stars, consistent with the common criterion . Possible observations of the radial oscillation frequencies could help to learn more about the equation of state, predict the maximum mass of neutron stars more precisely, and indicate the presence of quark matter.
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