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The advent of helioseismology has determined in detail the average rotationrate of the Sun as a function of radius and latitude. These data immediatelyreveal two striking boundary layers of shear in the solar convection zone (CZ):a tachocline at the base, where the differential rotation of the CZ transitionsto solid-body rotation in the radiative zone, and a 35-Mm-thick near-surfaceshear layer (NSSL) at the top, where the rotation rate slows by about 5% withincreasing radius. Though asteroseismology cannot probe the differentialrotation of distant stars to the same level of detail that helioseismology canachieve for the Sun, it is possible that many cool stars with outer convectiveenvelopes possess similar differential rotation characteristics, including botha tachocline and a NSSL. Here we present the results of 3D global hydrodynamicsimulations of spherical-shell convection for a Sun-like star at differentlevels of density contrast across the shell. The simulations with highstratification possess characteristics of near-surface shear, especially at lowlatitudes. We discuss in detail the dynamical balance of torques giving rise tothe NSSL in our models and interpret what these balances imply for the realSun. We further discuss the dynamical causes that may serve to wipe outnear-surface shear at high latitudes, and conclude by offering some theories asto how this problem might be tackled in future work.

Exploring the Influence of Density Contrast on Solar Near-Surface Shear