# Fundamental and higher-order excited modes of radial oscillation of neutron stars for various types of cold nucleonic and hyperonic matter

## TL;DR

This study computes fundamental and excited radial oscillation modes of neutron stars using various realistic equations of state, revealing correlations that aid in constraining models and advancing neutron star asteroseismology.

## Contribution

It provides detailed calculations of oscillation modes for different EoS models, enhancing understanding of neutron star internal structure and dynamics.

## Key findings

- Correlation between oscillation frequency and adiabatic index
- Constraints on realistic EoS models from oscillation data
- Implications for neutron star asteroseismology

## Abstract

This research paper complements our earlier qualitative study of the effect of viscosity and thermal conductivity on the radial oscillation and relaxation of non-rotating neutron stars. The fundamental and first two lowest-frequency excited modes of radial oscillation have been computed in the high nuclear density regime for a set of seven realistic equations of state (EoS) as functions of central energy density. Various types of zero-temperature EoS of cold nucleonic and hybrid nucleon-hyperon-quark matter models are used in the inner core to determine the internal structure in and around the hydrostatic equilibrium states and investigate the influence of each EoS on the dynamical behaviour of non-rotating neutron stars. We confirm the principal results of earlier, related studies that suggest an underlying correlation between the frequency spectrum of the fundamental oscillation mode and the variation of the adiabatic index over the high nuclear-density regime. We provide valuable information to impose further constraints on the plausible set of realistic EoS models, in addition to the practical applications for the rapidly evolving field of asteroseismology of compact objects.