Spin-down by dynamo action in simulated radiative stellar layers

TL;DR

This paper uses numerical simulations to demonstrate a magnetic dynamo mechanism in radiative stellar layers, which could explain internal magnetic fields and angular momentum transport without surface magnetic signatures.

Contribution

It identifies a subcritical dynamo transition in radiative zones, supporting the Tayler-Spruit dynamo theory and revealing a process for internal magnetic field generation in stars.

Findings

Supports the Tayler-Spruit dynamo mechanism

Generates deep toroidal magnetic fields

Enhances angular momentum transport in radiative zones

Abstract

The evolution of a star is influenced by its internal rotation dynamics through transport and mixing mechanisms, which are poorly understood. Magnetic fields can play a role in transporting angular momentum and chemical elements, but the origin of magnetism in radiative stellar layers is unclear. Using global numerical simulations, we identify a subcritical transition to turbulence due to the generation of a magnetic dynamo. Our results have many of the properties of the theoretically-proposed Tayler-Spruit dynamo mechanism, which strongly enhances transport of angular momentum in radiative zones. It generates deep toroidal fields that are screened by the stellar outer layers. This mechanism could produce strong magnetic fields inside radiative stars, without an observable field on their surface.