Magnetic flux in the solar convective envelope inferred from the initial magnetic flux of the sunspots

The initial measurements of rotation rate and magnetic flux of the sunspots that have different life spans and appear very first on the surface can be used for inferring radial variation of internal rotation and magnetic flux profiles in the solar convective envelope. In the present study, six year (1999-2004) SOHO/MDI magnetograms are used for the measurement of initial magnetic flux of the sunspots that appear very first on the solar surface and preliminary results are : (i) majority of the spot groups that have initial appearance on the surface are bipolar, (ii) irrespective of their sizes, the bipolar spots with different life spans have similar magnetic field strengths of 50 G during their first appearance on the surface, (iii) the field strength at the site of anchoring depths of the sunspots is estimated to be 10^5 G near base and 10^4 G near the surface, (iv) the dynamo-a source of sunspot activity-distributed through out the convective envelope and, (v) the rate of flux emergence of such a distributed dynamo is very high near base of the convective envelope compared to near the surface.