A first family of stable configurations to model magnetic fields in stellar radiation zones

TL;DR

This paper uses 3D MHD simulations to verify the stability of a theoretically derived magnetic field configuration in stellar radiation zones, supporting its use in modeling stellar magnetic phenomena.

Contribution

It demonstrates the stability of a specific magnetic equilibrium configuration in stellar radiation zones, validating its application in future stellar MHD simulations.

Findings

The configuration is stable under 3D MHD simulations.

It emphasizes the importance of non force-free properties.

Provides a model for initializing magnetic topology in stellar models.

Abstract

We conduct 3D magneto-hydrodynamic (MHD) simulations in order to test the stability of the magnetic equilibrium configuration described by Duez & Mathis (2010). This analytically-derived configuration describes the lowest energy state for a given helicity in a stellar radiation zone. The necessity of taking into account the non force-free property of the large-scale, global field is here emphasized. We then show that this configuration is stable. It therefore provides a useful model to initialize the magnetic topology in upcoming MHD simulations and stellar evolution codes taking into account magneto-rotational transport processes.