Differential Rotation in Solar Convective Dynamo Simulations
Abstract
We carry out a magneto-hydrodynamic (MHD) simulation of convective dynamo in the rotating solar convective envelope driven by the solar radiative diffusive heat flux. The simulation is similar to that reported in Fan & Fang (2014) but with further reduced viscosity and magnetic diffusion. The resulting convective dynamo produces a large scale mean field that exhibits similar irregular cyclic behavior and polarity reversals, and self-consistently maintains a solar-like differential rotation. The main driver for the solar-like differential rotation (with faster rotating equator) is a net outward transport of angular momentum away from the rotation axis by the Reynolds stress, and we found that this transport is enhanced with reduced viscosity and magnetic diffusion.
Cite
@article{arxiv.1512.08038,
title = {Differential Rotation in Solar Convective Dynamo Simulations},
author = {Yuhong Fan and Fang Fang},
journal= {arXiv preprint arXiv:1512.08038},
year = {2016}
}
Comments
27 pages, 11 figures, accepted for publication in Advances in Space Research