Rotation period as a function of latitude at different solar radii (r = 1.03,  2.0,  4.0,  8.0 and 16 R_⊙, from darker to lighter green lines) for the runs represented in Fig. 1 (from left to right: solar minimum, maximum, and decay phase; differential surface rotation on the top row, solid-body rotation on the bottom row). The red curves indicate the rotation period imposed at the surface (Eq. (6), with Ω_b and Ω_c having values of 0 in the solid rotation case). Rotation periods peak just outside CH–streamer boundaries, as in the UVCS observations by Giordano & Mancuso (2008). Global (resonant) oscillations of closed loops within the streamers are visible within these main peaks, especially in the case with differential rotation. Maximum rotational shearing occurs at mid-altitudes (below maximum streamer height). Wind shear is transmitted upwards, well above the streamer heights, at the vicinity of HCSs. At greater heights, the corona tends to progressively approach solid-body rotation with height within coronal holes (please note that the case in the third column has a polar pseudo-streamer).