Quasi-radial modes of pulsating neutron stars: numerical results for general-relativistic rigidly rotating polytropic models

TL;DR

This paper calculates how rigid rotation affects the pulsation eigenfrequencies of relativistic neutron star models, providing insights into their stability and oscillation characteristics.

Contribution

It presents numerical results for the change in pulsation eigenfrequencies due to rotation in general-relativistic polytropic neutron star models, including second-order rotational effects.

Findings

Eigenfrequency shifts due to rotation are quantified.

Rotation influences neutron star stability analysis.

Results aid in understanding pulsar oscillations.

Abstract

In this paper we compute general-relativistic polytropic models simulating rigidly rotating, pulsating neutron stars. These relativistic compact objects, with a radius of $\sim 10 \, \mathrm{km}$ and mass between $\sim 1.4$ and $3.2$ solar masses, are closely related to pulsars. We emphasize on computing the change in the pulsation eigenfrequencies owing to a rigid rotation, which, in turn, is a decisive issue for studying stability of such objects. In our computations, we keep rotational perturbation terms of up to second order in the angular velocity.