The imprint of the equation of state on the axial w-modes of oscillating neutron stars

TL;DR

This paper investigates how the internal equation of state of neutron stars influences their axial quasi-normal mode frequencies, suggesting gravitational wave detection could reveal details about neutron star matter and hadronic interactions.

Contribution

It demonstrates the dependence of neutron star oscillation frequencies on the equation of state using the continued fraction method across various models.

Findings

Detection of axial gravitational waves can distinguish between different equations of state.

Neutron star oscillation frequencies vary significantly with the stiffness of the equation of state.

Results provide insights into neutron star matter and hadronic interactions.

Abstract

We discuss the dependence of the pulsation frequencies of the axial quasi-normal modes of a nonrotating neutron star upon the equation of state describing the star interior. The continued fraction method has been used to compute the complex frequencies for a set of equations of state based on different physical assumptions and spanning a wide range of stiffness. The numerical results show that the detection of axial gravitational waves would allow to discriminate between the models underlying the different equation of states, thus providing relevant information on both the structure of neutron star matter and the nature of the hadronic interactions.