Magnetic Flux in the Solar Convective Envelope Inferred From the Sunspots' Initial Appearances (P27)

Details Magnetic Flux in the Solar Convective Envelope Inferred From the Sunspots' Initial Appearances (P27) Magnetic Flux in the Solar Convective Envelope Inferred From the Sunspots' Initial Appearances (P27)

Nov 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006ihy..worke.119l&link_type=abstract

2nd UN/NASA Workshop on International Heliophysical Year and Basic Space Science. Proceedings of the conference held 27 Novembe

Astronomy and Astrophysics

Astrophysics

Scientific paper

Sunspots with different life spans suggest their origin at different depths. By measuring magnetic fluxes from their first observation on the surface, one can estimate the strength of magnetic flux at different anchoring depths in the solar convective envelope. We measure initial fluxes of the sunspots on the solar surface using SOHO/MDI magnetograms. Hiremath’s (A&A, 386, 674, 2002) sunspots “life span-anchoring depth” information in the solar convective envelope and Parker’s (ApJ, 121, 491,1955) flux tube model are used for the estimation of the strength of the magnetic flux and the rate of emergence of magnetic flux at different anchoring depths. Important findings are: (i) majority of the spot groups that have first appearances on the surface are bipolar, (ii) irrespective of their sizes, the bipolar spots with different life spans have average magnetic field strengths of ~ 600G during their first observation,(iii) With a view to measure the strength of initial magnetic fluxes for a long stretch of Greenwich sunspot data, the initial area magnetic flux relationship is obtained, (iv) the average field strength at the site of anchoring depths of the sunspots is estimated to be ~106 G near base of the convective envelope and ~ 104 G near the surface, (v) the dynamo-a source of sunspot activity-is distributed through out the convective envelope, (vi) the rate of emergence of initial magnetic flux of such a distributed dynamo near base of the convection zone is 1019 Mx/day and is two times the rate of emergence of initial magnetic flux near the surface.

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