Nonlinear Decay of r modes in Rapidly Rotating Neutron Stars

TL;DR

This study uses 3D relativistic hydrodynamical simulations to explore the nonlinear decay and stability of r modes in rapidly rotating neutron stars, revealing decay timescales, differential rotation development, and effects of rotation rate.

Contribution

It provides the first detailed nonlinear analysis of r modes in rapidly rotating neutron stars using relativistic simulations, including eigenfunctions and decay behavior.

Findings

R modes decay in about ten oscillation periods at high amplitudes.

Stable r modes persist at amplitudes around unity.

Increased rotation rate slows down r-mode decay.

Abstract

We investigate the dynamics of r modes at amplitudes in the nonlinear regime for rapidly but uniformly rotating neutron stars with a polytropic equation of state. For this, we perform three-dimensional relativistic hydrodynamical simulations, making the simplifying assumption of a fixed spacetime. We find that for initial dimensionless amplitudes around three, r modes decay on timescales around ten oscillation periods, while at amplitudes of order unity, they are stable over the evolution timescale. Together with the decay, a strong differential rotation develops, conserving the total angular momentum, with angular velocities in the range 0.5..1.2 of the initial one. By comparing two models, we found that increasing rotation slows down the r-mode decay. We present r-mode eigenfunctions and frequencies, and compare them to known analytic results for slowly rotating Newtonian stars. As a diagnostic tool, we discuss conserved energy and angular momentum for the case of a fixed axisymmetric background metric and introduce a measure for the energy of non-axisymmetric fluid oscillation modes.