||Global-Scale Simulations of Stellar Convection and Their Observational Predictions
||487, Resolving The Future Of Astronomy With Long-Baseline Interferometry
||Brown, B. P.
||Stars on the lower main sequence (F-type through M-type) have
substantial convective envelopes beneath their stellar photospheres.
Convection in these regions can couple with rotation to build
global-scale structures that may be observable by interferometers that
can resolve stellar disks.
Here I discuss predictions emerging from 3D MHD simulations
for solar-type stars with the anelastic spherical harmonic (ASH) code
and how these predictions may be observationally tested.
The zonal flow of differential rotation is likely the most
easily observable signature of dynamics occuring deep within the
Generally, we find that rapidly rotating suns have a strong solar-like
differential rotation with a prograde equator and retrograde poles,
while slowly spinning suns may have anti-solar rotation profiles with
fast poles and slow equators. The thermal wind balance accompanying
the differential rotation may lead to hot and bright poles in the
rapid rotators and cooler, darker poles in slow rotators. The
convection and differential rotation build global-scale magnetic
structures in the bulk of the convection zone, and these wreaths of
magnetism may be observable near the stellar surfaces.