Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.2235c&link_type=abstract
American Astronomical Society, SPD meeting #42, #22.35; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
The electric field in the reconnecting current sheet is estimated from the change rate of photospheric magnetic flux in the newly brightened areas of TRACE UV ribbons. The X10 flare on 2003 October 29 is selected due to its distinct two-phase HXR footpoint motion, two arcade systems with different magnetic shear, and the high-cadence and complete coverage of TRACE 1600 Å, MDI magnetogram, and RHESSI HXR observations. Besides the strengths of reconnection electric field in different flare phases, we particularly pay attention to the temporal correlation between the reconnection electric field and the corresponding characteristics at the conjugate HXR footpoints (such as the HXR emissions, HXR power-law spectral indexes, and the photospheric magnetic field strengths). We found that in the early impulsive phase, the reconnection electric field peaks just before the HXR emission peaks and the energy spectrum hardens. The result could be consistent with the scenario that more particles are accelerated to higher energies by larger reconnection electric field and then precipitate into lower chromosphere to produce stronger HXR emissions. Moreover, such particle acceleration mechanism plays most significant role in the impulsive phase of this X10 flare. In addition, our results provide the evidence that the highly-sheared magnetic field lines are mapped to the magnetic reconnection diffusion region to produce large reconnection electric field.
Cheng C. Z.
Hsieh Michael
Krucker Sa"m
Yang Yan-Hong
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