Gravitational Wave Generation in Rotating Compact Stars

TL;DR

This paper models gravitational wave emission from rotating neutron stars using a simplified triaxial ellipsoid approach, deriving the radiation rate and numerically solving the star's evolution with neutrino diffusion.

Contribution

It introduces an effective Lagrangian model for rotating neutron stars and incorporates neutrino diffusion in the numerical analysis of gravitational wave emission.

Findings

Derived the gravitational wave radiation rate in the weak field limit.

Numerically solved the star's evolution including neutrino diffusion.

Provided insights into the main aspects of neutron star gravitational wave emission.

Abstract

We present a simplified description of a rotating neutron star emitting gravitational waves. We describe the system by an uniformly rotating triaxial homogeneous ellipsoid to catch the main aspects of the evolution. We construct an effective Lagrangian model, in which the kinetic energy associated to the breath mode and rotation are explicitly determined. The rate of gravitational waves radiation is determined in the framework of the weak field limit approximation of Einstein equations. We then solve numerically the equations of motion for the nascent neutron star, incorporating the diffusion of neutrinos in the calculation.