Magnetic Field Topology and the Thermal Structure of the Corona over Solar Active Regions

Details Magnetic Field Topology and the Thermal Structure of the Corona over Solar Active Regions Magnetic Field Topology and the Thermal Structure of the Corona over Solar Active Regions

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21631201s&link_type=abstract

American Astronomical Society, AAS Meeting #216, #312.01; Bulletin of the American Astronomical Society, Vol. 41, p.887

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Solar extreme-ultraviolet images of active-region coronae are characterized by ensembles of bright 1-2 MK loops that fan out from select locations. We investigate the conditions associated with the formation of these relatively cool loop fans within the otherwise 3-5 MK coronal environment by combining EUV observations of active regions made with the Transition Region and Coronal Explorer (TRACE) with global source-surface potential-field models based on the full-sphere photospheric field from the assimilation of magnetograms that are obtained by MDI on SOHO. We find that in the selected active regions with largely potential field configurations these fans are associated with (quasi-)separatrices within the strong-field regions of magnetic plage and vice versa. We argue that the divergence of the field lines across a (quasi-)separatrix may cause heating to happen relatively low in the corona, resulting in a lower loop temperature and flatter thermal profile of relatively dense (and thus EUV-bright) loops that are surrounded by warmer, thermally more stratified loops in field that does not straddle such topological divides.

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