Breaking Taylor-Proudman balance by magnetic field in stellar convection zone

Abstract

We carry out high-resolution calculations for the stellar convection zone. The main purpose of this study is to investigate the effect of a small-scale dynamo on the differential rotation. The solar differential rotation deviates from the Taylor-Proudman state in which the angular velocity does not change along the rotational axis. To break the Taylor-Proudman state deep in the convection zone, it is thought that a latitudinal entropy gradient is required. In this study, we find that the small-scale dynamo has three roles in the deviation of the stellar differential rotation from the Taylor-Proudman state. 1. The shear of the angular velocity is suppressed. This leads to a situation where the latitudinal entropy gradient efficiently breaks the Taylor-Proudman state. 2. The perturbation of the entropy is increased with suppressing the turbulent velocity between up- and downflows. 3. The convection velocity is reduced. This increases the effect of the rotation on the convection. The second and third factors increase the latitudinal entropy gradient and break the Taylor-Proudman state. We find that the efficient small-scale dynamo has a significant impact on the stellar differential rotation.

18 pages, 5 figures, accepted for publication in The Astrophysical Journal Letters

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• Implicit large eddy simulations of global solar convection: effects of numerical resolution in non-rotating and rotating cases
• Magnetic Taylor-Proudman constraint explains the flows into the Tangent Cylinder
• Discovery of new magnetic δ Scuti stars and impact of magnetism on pulsation excitation