Solar transition region reconnection

Details Solar transition region reconnection Solar transition region reconnection

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh24a..08b&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH24A-08

Physics

7509 Corona, 7843 Numerical Simulation Studies, 6050 Plasma And Mhd Instabilities, 2772 Plasma Waves And Instabilities, 3210 Modeling

Scientific paper

In order to identify the primary sites of coronal heating caused by a relaxation of the currents which are due to the footpoint motion of magnetic loops we developed a special MHD simulation approach which utilizes plasma-physical results about current dissipation, starting with observed photospheric magnetic fields and their displacements. Using photospheric magnetic fields measured by SOHO's MDI we obtained that the most intensive reconnection processes take place at the transition region between the chromosphere and corona, where the plasma density drops and the temperature jumps up. As the reason for this effect we identified the enhanced velocity of the current carriers concentrated in thin sheets at the edge of the chromosphere which exactly there causes collisionless current dissipation and, finally, reconnection.

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