Analysis of 3D MHD Instability of Antisolar Latitudinal Differential Rotation in F, G and K stars
Mausumi Dikpati, Paul S. Cally

TL;DR
This study investigates the stability of antisolar and solar differential rotations in F, G, and K stars' tachoclines, revealing that antisolar rotation is generally more unstable and weaker, especially in F stars, which may explain observed weak antisolar rotations.
Contribution
The paper introduces a detailed stability analysis of antisolar differential rotation in stars using two advanced 3D thin shell models, highlighting the instability's role in weak antisolar rotations.
Findings
Antisolar differential rotation is more unstable than solar type.
Instability tends to weaken antisolar differential rotation.
Weak antisolar rotations are more likely in F stars with thinner convection zones.
Abstract
Motivated by observations that only a very few stars have been found to have antisolar differential rotation, much weaker in amplitude than that of the Sun, we analyze the stability of antisolar and solar type latitudinal differential rotations in the tachoclines of typical F,G and K stars. We employ two three-dimensional thin shell models, one for a Boussinesq but non-hydrostatic system, the other for a hydrostatic but non-Boussinesq system. We find that, in general, the combination of toroidal field band and differential rotation is more unstable, and unstable for lower toroidal fields, for antisolar than for solar-type differential rotation. In the antisolar case, the instability is always found to weaken the differential rotation, even if the primary energy source for the instability is the magnetic field. This favors surface antisolar differential rotations in stars being weaker…
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