Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.0903g&link_type=abstract
American Astronomical Society, SPD meeting #42, #9.03; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
For the past nine years, hard X-ray observations by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) have provided remarkable insight into the locations and spectra of energetic flare particles. With the advent of high-cadence, multiwavelength observations by the Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory, it is now possible to study the dynamic structures among which these energetic particles move. On November 3, 2010, a C4.9 solar flare emerged from behind the eastern limb of the Sun, accompanied by a coronal mass ejection. Because the bright flare footpoints were occulted by the solar disk (by about 12 degrees), the coronal X-ray sources can be studied in detail without contamination by the footpoints. Extreme ultraviolet (EUV) images from AIA show a mass of plasma ejected from the solar surface. Isothermal analysis using multiple EUV filters shows that this erupting plasma reaches a high temperature of 11 MK. Meanwhile, RHESSI X-ray images reveal a large, diffuse hard X-ray source that matches the location and shape of the ejecting plasma, suggesting the presence of nonthermal electrons magnetically trapped in the region. Using RHESSI spectroscopy and AIA temperature analysis, we will test the hypothesis that nonthermal electrons in the erupting plasma are responsible for heating the plasma to this high temperature via collisional heating.
Bain Hazel M.
Glesener Lindsay
Krucker Sa"m
Lin Robert P.
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