Evolution of Active Regions in the Solar Interior

Details Evolution of Active Regions in the Solar Interior Evolution of Active Regions in the Solar Interior

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh22a0186k&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH22A-0186

Physics

7522 Helioseismology, 7536 Solar Activity Cycle (2162), 7544 Stellar Interiors And Dynamo Theory

Scientific paper

Using data from SOHO and TRACE, we investigate the emergence, evolution and dissipation of magnetic active regions in the solar interior and atmosphere by comparing 3D maps of subsurface structures and plasma flows, obtained by acoustic tomography, with the corresponding photospheric magnetograms and coronal EUV images. We find that the growth of active regions is characterized by multiple emergence of magnetic flux structures propagating very rapidly in the upper convection zone and by the formation of large-scale converging flows. During the decay, we have observed mostly diverging flows, and have attempted to detect submergence of magnetic flux. We look at some details of the dynamics of active regions, and discuss initial results of a search for the relationship between subphotospheric shearing flows, and changes in magnetic topology and flaring activity in the corona.

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