Influence of the nuclear matter equation of state on the r-mode instability using the finite-range simple effective interaction

TL;DR

This paper investigates how the nuclear matter equation of state influences the r-mode oscillation properties of rotating neutron stars, focusing on the effects of the stiffness of nuclear interactions on r-mode amplitude limits.

Contribution

It introduces a detailed analysis of the impact of the nuclear equation of state on neutron star r-modes using the finite-range simple effective interaction model.

Findings

R-mode saturation amplitude upper limit is between 10^{-8} and 10^{-6}.

The stiffness of nuclear matter affects the physical properties of neutron star oscillations.

Results align with previous predictions on r-mode amplitudes.

Abstract

The characteristic physical properties of rotating neutron stars under the r-mode oscillation are evaluated using the finite-range simple effective interaction. Emphasis is given on examining the influence of the stiffness of both the symmetric and asymmetric parts of the nuclear equation of state on these properties. The amplitude of the r-mode at saturation is calculated using the data of particular neutron stars from the considerations of "spin equilibrium" and "thermal equilibrium". The upper limit of the r-mode saturation amplitude is found to lie in the range 10^{-8}-10^{-6}, in agreement with the predictions of earlier work.