Stability of magnetic fields in non-barotropic stars: an analytic treatment

TL;DR

This paper provides an analytic study of magnetic field stability in non-barotropic stars, showing how mixed poloidal and toroidal fields can be stable and potentially power magnetar activity.

Contribution

It derives an explicit equilibrium structure for magnetic fields in non-barotropic stars and analyzes their stability using the energy principle, confirming the stabilizing role of poloidal fields.

Findings

Toroidal fields can be stabilized by weaker poloidal fields.

Stable stratification allows for a wider range of magnetic configurations.

Toroidal fields may power magnetar activity and emit gravitational waves.

Abstract

Magnetic fields in upper main-sequence stars, white dwarfs, and neutron stars are known to persist for timescales comparable to their lifetimes. From a theoretical perspective this is problematic, as it can be shown that simple magnetic field configurations are always unstable. In non-barotropic stars, stable stratification allows for a much wider range of magnetic field structures than in barotropic stars, and helps stabilize them by making it harder to induce radial displacements. Recent simulations by Braithwaite and collaborators have shown that, in stably stratified stars, random initial magnetic fields evolve into nearly axisymmetric configurations with both poloidal and toroidal components, which then remain stable for some time. It is desirable to provide an analytic study of the stability of such fields. We write an explicit expression for a plausible equilibrium structure of an axially symmetric magnetic field with both poloidal and toroidal components of adjustable strengths, in a non-barotropic static fluid star, and study its stability using the energy principle. We construct a displacement field that should be a reasonable approximation to the most unstable mode of a toroidal field, and confirm Braithwaite's result that a given toroidal field can be stabilized by a poloidal field containing much less energy than the former. This is consistent with the speculation that the toroidal field is the main reservoir powering magnetar activity. The deformation of a neutron star caused by the hidden toroidal field can also cause emission of gravitational waves.