HR: 1330h
AN: SH22A-0168    [PDF]
TI: Gamma-ray flare occurrence patterns
AU: * Hudson, H S
EM: hhudson@ssl.berkeley.edu
AF: SSL, 7 Gauss Way UCB, Berkeley, CA 94720-7450 United States
AU: Lin, R P
EM: boblin@ssl.berkeley.edu
AF: SSL, 7 Gauss Way UCB, Berkeley, CA 94720-7450 United States
AU: Smith, D M
EM: dsmith@ssl.berkeley.edu
AF: SSL, 7 Gauss Way UCB, Berkeley, CA 94720-7450 United States
AB: 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.
DE: 7509 Corona
DE: 7513 Coronal mass ejections
DE: 7519 Flares
DE: 7554 X rays, gamma rays, and neutrinos
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting