Zoomed-in view of the absolute magnitudes of the gradients of flow speed (top) and of the rotation rate Ω (bottom) close to the equatorial streamer on the solar minimum (left) and maximum (right) configurations. For simplicity, only differentially rotating cases are shown, and both quantities are displayed in normalised units (in units of 6.27 × 10⁻⁴ s⁻¹ and 9.0 × 10⁻¹³ rad s⁻¹ m⁻¹, respectively). The axis indicates distances in solar radii. The green lines are magnetic field lines. The coronal hole–streamer boundaries systematically develop flow shears because of the gradients the solar wind speed (flow along the magnetic field) and of the gradients in the rotation pattern (flow across the field) combined. These shearing regions reach well into the coronal holes, and into the wind flow well past the streamer top height.