Magnetic Nonpotentiality Accumulation Prior to a "Large" B1.7 Two-Ribbon Flare

Details Magnetic Nonpotentiality Accumulation Prior to a "Large" B1.7 Two-Ribbon Flare Magnetic Nonpotentiality Accumulation Prior to a "Large" B1.7 Two-Ribbon Flare

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.2002s&link_type=abstract

American Astronomical Society, SPD meeting #40, #20.02; Bulletin of the American Astronomical Society, Vol. 41, p.852

Astronomy and Astrophysics

Astronomy

Scientific paper

A B1.7 two-ribbon flare occurred in a highly non-potential decaying active region near a coronal hole at 10:00 UT on May 17, 2008. This flare is "large" in the sense that it involves the entire region, and it is associated with both a filament eruption and a CME. We present multi-wavelength observations from EUV (TRACE, STEREO/EUVI), X-rays (Hinode/XRT), and H-alpha (THEMIS, BBSO) prior to, during and after the flare. Prior to the flare, the observed coronal loops are mainly two sets of highly sheared loops surrounding two filaments. The sheared loops in the southern part of the region appeared in TRACE around 22:00 UT after a filament ejection on May 16. We also performed non-linear force free field (NLFFF) modeling for the region prior to the flare, using the flux rope insertion method. The model at 11:42 UT on May 16 is based on THEMIS (vector) and MDI magnetograms, and the model at 08:03 UT on May 17 is based only on MDI magnetogram. The best-fit NLFFF models show good fit to observations both in the corona (X-ray and EUV loops) and chromosphere (H-alpha filament). In the photosphere, the vectors in the best-fit NLFFF model are similar to those in the potential model. However, in the chromosphere, the vectors in the best-fit NLFFF model present strong non-potentiality, especially at the end of the inserted flux rope. We also found that the axial flux of the flux rope in the NLFFF model on May 17 is much higher than that on May 16.

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