  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 occurring deep within the stellar
interior. 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.
