Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.1303f&link_type=abstract
American Astronomical Society, SPD meeting #42, #13.03; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
We present a 3D MHD simulation that qualitatively models the coronal magnetic field evolution of the eruptive flare occurred on December 13, 2006 in the emerging delta-sunspot region NOAA 10930 observed by the Hinode satellite. The simulation is set up where we drive the emergence of a twisted magnetic flux rope at the lower boundary into a pre-existing coronal potential field derived based on the MDI full-disk magnetogram at 20:51:01 UT on December 12, 2006. The resulting coronal flux rope embedded in the ambient coronal magnetic field first settles into a stage of quasi-static rise, and then undergoes a dynamic eruption, with the front of the flux rope cavity accelerating to a steady speed of about 900 km/s. The pre-eruption coronal magnetic field shows morphology that is similar to that seen in the Hinode soft X-ray observation of the region in both the magnetic connectivity as well as the development of a central inverse-S shaped X-ray sigmoid due to the formation of a current sheet underlying the flux rope. We examine the properties of the erupting flux rope and also the accompanying reconnections and the post-reconnection loops, and compare them with observations.
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