Left: comparison between the coronal residual rotation rates at 1.6 R_⊙ (red filled circles) and the solar rotation rates at three different depths below the photosphere (0.99, 0.95, and 0.90 R_⊙) retrieved from GONG and MDI data (blue open squares). Right: scatter plots showing the correlation between the residual rotation rates in the corona and below the photosphere in the upper layers of the convection zone of the Sun down to 0.90 R_⊙.