RHESSI and SDO Observation Of HXR and UV/EUV Emissions in the 2011 March 7 Solar Flare

Details RHESSI and SDO Observation Of HXR and UV/EUV Emissions in the 2011 March 7 Solar Flare RHESSI and SDO Observation Of HXR and UV/EUV Emissions in the 2011 March 7 Solar Flare

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.2231c&link_type=abstract

American Astronomical Society, SPD meeting #42, #22.31; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

We present analysis of the RHESSI and SDO observation of a very unusual M3.7 class solar flare on 2011 March 7 from the active region 11164, which was also detected by the Fermi Large Area Telescope above 100 MeV at gamma-rays and NoRP at microwaves. This flare was accompanied by a relatively strong CME and solar energetic particles.
During the flare, hard X-ray emission up to 300 keV was detected by RHESSI. The HXR images at 12-300 keV in the impulsive phase exhibit two footpoint sources with an unusually large separation of more than 120 arcsec and a thermal loop below 18 keV connecting the two footpoints. On the other hand, the SDO/AIA UV and EUV images indicate that the spatial structure of the flare is much more complicated than the above HXR picture. The UV continuum images at 1600 and 1700 angstrom show three elongated ribbons, the outer two being brightest and coincident with the HXR footpoints and the middle one without any detectable cospatial HXR source. Furthermore, the EUV images show a few arcade systems successively developing during the flare, while there are no clear EUV loops seen to connect the two HXR footpoints.
We will examine the magnetic configuration within the flaring regions using the RHESSI, SDO/AIA and SDO/HMI magnetogram data, and investigate the relation between UV ribbon brightening and electron heating in this flare. The relation between the HXR and EUV emission and other observations will be analyzed and described.

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