Gamma-ray flare occurrence patterns

Details Gamma-ray flare occurrence patterns Gamma-ray flare occurrence patterns

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh22a0168h&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH22A-0168

Statistics

7509 Corona, 7513 Coronal Mass Ejections, 7519 Flares, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

As of 2003 September 4, RHESSI (the Reuven Ramaty High-Energy Spectroscopic Imager) had obtained coverage for the entire GOES duration (>95%) for 98 M- and 6 X-class flares, and for each of these we estimate the ratio of the 2.223 MeV line fluence to the GOES soft X-ray fluence. All are upper limits except for one M-class event and one X-class event. The GOES fluence is known to scale well with total flare energy. The statistics of these observations, considering as well the solar gamma-ray line observations from other spacecraft plus the statistics of proton events in the heliosphere, are not consistent with the hypothesis that ion acceleration scales proportionally with total flare energy.

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