Magnetic fields generated by r-modes in accreting millisecond pulsars

TL;DR

This paper explores how r-modes in accreting millisecond pulsars can generate strong magnetic fields through differential rotation, affecting the star's stability and evolution.

Contribution

It introduces the magnetic damping rate into r-mode evolution equations and demonstrates magnetic field generation in neutron star cores for the first time.

Findings

R-modes can induce strong toroidal magnetic fields in neutron stars.

Magnetic fields influence the stability and long-term evolution of pulsars.

The study provides insights into magnetic stabilization mechanisms.

Abstract

In rotating neutron stars the existence of the Coriolis force allows the presence of the so-called Rossby oscillations (r-modes) which are know to be unstable to emission of gravitational waves. Here, for the first time, we introduce the magnetic damping rate in the evolution equations of r-modes. We show that r-modes can generate very strong toroidal fields in the core of accreting millisecond pulsars by inducing differential rotation. We shortly discuss the instabilities of the generated magnetic field and its long time-scale evolution in order to clarify how the generated magnetic field can stabilize the star.