Waves in the radiative zones of rotating, magnetized stars

TL;DR

This paper develops an asymptotic theory for short-wavelength waves in the radiative zones of rotating, magnetized stars, exploring how magnetic fields influence oscillation modes using a Hamiltonian ray-tracing approach.

Contribution

It introduces a new asymptotic framework and dispersion relation for magnetized, rotating stellar radiative zones, incorporating complex magnetic topologies.

Findings

Magnetic fields significantly alter gravito-inertial wave properties.

The Hamiltonian ray-tracing method reveals magnetic topology effects.

The dispersion relation provides insights into wave behavior in magnetized stars.

Abstract

Asteroseismology has reached a level of accuracy that may allow us to detect the effect of a deep magnetic field on oscillation modes. We thus aim to develop an asymptotic theory for short-wavelength waves in radiative zones of rotating stars with a general magnetic field topology (toroidal and poloidal). A dispersion relation is derived for a uniformly rotating star with a low-amplitude, axisymmetric magnetic field. The parameter space of this model is explored with a Hamiltonian ray-tracing method. The features of the gravito-inertial waves modified by the magnetic field are studied with different magnetic topologies.