The rotation rate of the solar radiative zone

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.

Submitted to ApJ

References in corpus (4)

• Magnetic confinement of the solar tachocline
• Dynamics of the solar tachocline II: the stratified case
• On the penetration of meridional circulation below the solar convection zone
• Spherical Couette flow in a dipolar magnetic field

Cited by in corpus (6)

• Solar structure and evolution
• Dynamics of the solar tachocline III: Numerical solutions of the Gough and McIntyre model
• On the Penetration of Meridional Circulation below the Solar Convection Zone II: Models with Convection Zone, the Taylor-Proudman constraint and Applications to Other Stars
• Some glimpses from helioseismology at the dynamics of the deep solar interior
• Magnetic activity, differential rotation and dynamo action in the pulsating F9IV star KIC 5955122
• A semi-analytic approach to angular momentum transport in stellar radiative interiors