Relations Between Concurrent Hard X-ray Sources In Solar Flares

Details Relations Between Concurrent Hard X-ray Sources In Solar Flares Relations Between Concurrent Hard X-ray Sources In Solar Flares

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.2801b&link_type=abstract

American Astronomical Society, SPD meeting #37, #28.01; Bulletin of the American Astronomical Society, Vol. 38, p.254

Astronomy and Astrophysics

Astronomy

Scientific paper

Solar flares release a large fraction of their energy into non-thermal electrons,but it is not clear where and how. Bremsstrahlung X-rays are observed from the corona (coronal or looptop source) and chromosphere (footpoints).The spectral time evolution of the sources and the relations between themreflect the geometry and constrict the configuration of the flare.We studied solar flares of GOES class larger than M1 with three hard X-raysources observed simultaneously in the course of the flare. The events whereselected from observations with the X-ray satellite RHESSI from February 2002 until July 2005.We used imaging spectroscopy methods to determine the spectral time evolution ofeach source in each event. The images of all of the five events show twosources visible only at high energies (footpoints) and one source onlyvisible at low energies (coronal source).We find soft-hard-soft behavior in both, coronal source and footpoints. Thisis a strong indication that soft-hard-soft is a feature of the accelerationmechanism rather than a transport effect.The coronal source is nearly always softer than the footpoints. The footpointspectra differ significantly only in one event out of five.

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