Partially Occulted Flares versus Disk Flares in YOHKOHDatabase

Details Partially Occulted Flares versus Disk Flares in YOHKOHDatabase Partially Occulted Flares versus Disk Flares in YOHKOHDatabase

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...122.104t&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

Among from 1286 flares in the YOHKOH Hard X-ray Telecope Flare Catalogue (Sato et al. 2006, Solar Phys., 236, 351), for which the hard X-ray images have been enclosed, we identified 98 events that occurred behind the solar limb. We found that photon energy spectra of partially occulted flares are systematically steeper than spectra of disk flares (average values of the power-law index differ of about 2). Such a difference we explain as a consequence of intrisically dissimilar conditions ruling in a coronal part of flares in comparison with the footpoints which usually dominate the hard X-ray emission of disk flares. At least two reasons should be taken into consideration: (1) stronger contamination of thermal plasma, (2) different mechanism in which non-thermal electrons radiate their energy. A few partially occulted flares showing flat photon energy spectra was related to a progressive spectral hardening.

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