Tayler–Spruit dynamo simulations for the modeling of radiative stellar layers

¹ LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université, Paris, France
e-mail: ludovic.petitdemange@obspm.fr
² Université Côte d’Azur, Inria, CNRS, LJAD, France
e-mail: florence.marcotte@inria.fr
³ LPENS, Laboratoire de Physique de l’École Normale Supérieure, ENS, Université PSL, CNRS, Institut Universitaire de France, Paris, France
e-mail: christophe.gissinger@phys.ens.fr
⁴ LPENS Laboratoire de Physique de l’École Normale Supérieure, ENS, Université PSL, CNRS, Paris, France

Received: 20 June 2023
Accepted: 18 October 2023

Abstract

Context. Maxwell stresses exerted by dynamo-generated magnetic fields have been proposed as an efficient mechanism to transport angular momentum in radiative stellar layers. Numerical simulations are still needed to understand its trigger conditions and the saturation mechanisms.

Aims. The present study follows up on a recent paper where we reported on the first simulations of Tayler-Spruit dynamos. Here we extend the parameter space explored to assess in particular the influence of stratification on the dynamo solutions. We also present numerical verification of theoretical assumptions made previously that were instrumental in deriving the classical prescription for angular momentum transport implemented in stellar evolution codes.

Methods. A simplified radiative layer is modeled numerically by considering the dynamics of a stably stratified, differentially rotating, magnetized fluid in a spherical shell.

Results. Our simulations display a diversity of magnetic field topologies and amplitudes depending on the flow parameters, including hemispherical solutions. The Tayler-Spruit dynamos reported here are found to satisfy magnetostrophic equilibrium and achieve efficient turbulent transport of angular momentum, following Spruit’s heuristic prediction.