Coronal Gamma-ray Sources in Solar Flares

Details Coronal Gamma-ray Sources in Solar Flares Coronal Gamma-ray Sources in Solar Flares

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9314k&link_type=abstract

American Astronomical Society Meeting 210, #93.14; Bulletin of the American Astronomical Society, Vol. 39, p.213

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Scientific paper

The Reuven Ramaty High Energy Spectroscopic Imager (RHESSI) provides for the first time imaging spectroscopy of solar flares up to the gamma-ray range. The three RHESSI flares with best counting statistics are analyzed in the 200-800 keV range revealing gamma-ray emission produced by electron bremsstrahlung from footpoints of flare loops, but also from the corona.Footpoint emission dominates during the gamma-ray peak, but as the gamma-ray emission decreases the coronal source becomes more and more prominent. Furthermore, the coronal source shows a much harder spectrum (with power law indices between 1.5 and 2) than the footpoints (with indices between 3 and 4). These observations suggest that flare-accelerated high energy electrons ( MeV) are staying long enough in the corona and lose their energy by collisions producing gamma-ray emission, while lower energetic electrons precipitate to the footpoints without losing significant energy in the corona.

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