Sample results from tests that were performed to assess the dependence on the layer thickness ΔR/R₁, number of layers N_r, and viscosity ν. Left: ω″ profiles for azimuth angles at which the most pronounced velocity gradients occur, computed with the combinations of ΔR/R₁, N_r, and ν as indicated by the legend which, from top to bottom, refers to cases to Cases 1, 2, 14, 11 and 3 in Table A.1. The abscissa is the radial distance from the center of the star to the layer midpoint. Right: Surface angular velocity from models holding all input parameters constant except for ν, showing that calculations with smaller values of ν reach the same rotation state as those with larger values, but after longer times. The three curves show: Top: Case 1 at Day 397 (green), Case 6 at Day 798 (black), Case 7 at Day 2004 (cyan). Middle: Case 7 at Day 798 (cyan), Case 8 at Day 8024 (red). Bottom: Case 6 at Day 36 (black), Case 8 at Day 2003 (red).