Helioseismic observations of developing active regions in the solar convection zone

Details Helioseismic observations of developing active regions in the solar convection zone Helioseismic observations of developing active regions in the solar convection zone

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.8903k&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #89.03; Bulletin of the American Astronomical Society, Vol. 34, p.791

Astronomy and Astrophysics

Astronomy

Scientific paper

Time-distance helioseismology provides unique opportunities for studying the formation and evolution of regions of solar activity. The key questions are: How deep in the convection zone are the active regions formed? How fast do they erupt? What is the role of convective mass flows in the formation and evolution of active regions? Is there retraction of magnetic flux during the decay of active regions? Why do new active regions tend to appear in places where previous active regions existed? We discuss the current techniques for probing the subphotospheric structure and dynamics of active regions, uncertainties and limitations of these studies, and present results of observation of three developing active regions using Michelson Doppler Imager on SOHO.

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