Poster abstract details

Sunspots that rotate around their vertical axis are classified as rotating sunspots. It is suggested that the origin of rotational motion is mainly due to the shear and twist in magnetic field lines or vice versa. It is also proposed that the magnetic twist may result from large-scale flows in the solar convection zone and the photosphere or in subphotospheric layers. We apply the technique of ring-diagrams to study the flows beneath these rotating sunspots and investigate how flow fields change with depth. We also study divergence and vorticity of horizontal flows and compare these with those for non-rotating sunspots.