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Magnetic field topology and the thermal structure of the corona over solar active regions View all abstracts by submitter

Karel Schrijver   Submitted: 2010-06-25 15:51

Solar extreme-ultraviolet images of quiescent active-region coronae are char- acterized by ensembles of bright 1 - 2 MK loops that fan out from select loca- tions. We investigate the conditions associated with the formation of these per- sistent, relatively cool loop fans within and surrounding the otherwise 3 - 5 MK coronal environment by combining extreme-ultraviolet (EUV) observations of ac- tive regions made with the Transition Region and Coronal Explorer (TRACE) with global source-surface potential-field models based on the full-sphere pho- tospheric field from the assimilation of magnetograms that are obtained by the Michelson Doppler Imager (MDI) on SOHO. We find that in the selected active regions with largely potential field configurations these fans are associated with (quasi-)separatrix layers (QSLs) within the strong-field regions of magnetic plage. Based on the empirical evidence, we argue that persistent active-region cool loop fans are primarily related to the pronounced change in connectivity across a QSL to widely separated clusters of magnetic flux, and confirm earlier work that sug- gested that neither a change in loop length nor in base field strengths across such topological features are of prime importance to the formation of the cool loop fans. We discuss the hypothesis that a change in the distribution of coronal heating with height may be involved in the phenomenon of relatively cool coronal loop fans in quiescent active regions.

Authors: Carolus J. Schrijver, Marc L. DeRosa, and Alan M. Title
Projects: TRACE

Publication Status: Astrophysical Journal, in press
Last Modified: 2010-06-28 09:15
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