The rotation rate of the solar radiative zone

TL;DR

This paper investigates the rotation rate of the solar radiative zone by analyzing viscous and magnetic stresses through analytical models, simulations, and observations to better understand angular-momentum transport.

Contribution

It introduces a simple linearized toy model to study the effects of magnetic field geometry and boundary conditions on the solar radiative zone's rotation profile.

Findings

Analytical predictions align with nonlinear simulations.

Magnetic stresses significantly influence the rotation rate.

Results provide constraints for solar interior models.

Abstract

The rotation rate of the solar radiative zone is an important diagnostic for angular-momentum transport in the tachocline and below. In this paper we study the contribution of viscous and magnetic stresses to the global angular-momentum balance. By considering a simple linearized toy model, we discuss the effects of field geometry and applied boundary conditions on the predicted rotation profile and rotation rate of the radiative interior. We compare these analytical predictions with fully nonlinear simulations of the dynamics of the radiative interior, as well as with observations. We discuss the implications of these results as constraints on models of the solar interior.