Solar Filament Evolution in the Presence of Subsurface Flows

Details Solar Filament Evolution in the Presence of Subsurface Flows Solar Filament Evolution in the Presence of Subsurface Flows

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.3202h&link_type=abstract

American Astronomical Society, SPD meeting #37, #32.02; Bulletin of the American Astronomical Society, Vol. 38, p.257

Astronomy and Astrophysics

Astronomy

Scientific paper

Many models of filament formation and evolution are driven by converging and shearing flows in the photosphere and upper convection zone, where the gas is dense enough to move the magnetic footpoints of a filament. With our recent development of High-Resolution Ring Analysis (HRRA) procedures, we are now able to measure flows below the surface with a horizontal resolution of 2 heliographic degrees (˜20 Mm). With this HRRA analysis of the flows underlying filaments and filament channels, we have found evidence of shearing flows along the neutral line in at least one instance and will be presenting the results from several more filaments. This research is funded in part by NASA grants NAG5-12491 and NNG05GM83G.

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