Differential Rotation and Magnetism in Simulations of Fully Convective Stars
Differential Rotation and Magnetism in Simulations of Fully Convective Stars
Abstract Stars of sufficiently low mass are convective throughout their interiors, and so do not possess an internal boundary layer akin to the solar tachocline. Because that interface figures so prominently in many theories of the solar magnetic dynamo, a widespread expectation had been that fully convective stars would exhibit …