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A. Y. Shih (Department of Physics and Space Sciences Laboratory, UC, Berkeley), D. M. Smith (Department of Physics and Santa Cruz Institute for Particle Physics, UC, Santa Cruz), R. P. Lin (Department of Physics and Space Sciences Laboratory, UC, Berkeley), R. A. Schwartz (NASA GSFC), G. H. Share, R. J. Murphy (E. O. Hulburt Center for Space Research, NRL)
The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) detected nuclear gamma-ray line emission from at least three of the X-class solar flares of October-November 2003: the X17 on October 28, the X11 on October 29, and the X8.3 on November 2. Collisions of accelerated ions with the ambient solar medium produce nuclear de-excitation lines, and the ratio of the fluxes in these lines depends on the acceleration spectrum and the composition of the medium. Earlier studies of the X4.8 solar flare on 2002 July 23 showed a significant change in the flux ratios as that flare progressed, which suggests a corresponding change in the circumstances of ion acceleration. We analyze these later flares for similar evidence of temporal variation.
The work at the University of California, Berkeley, was supported by NASA contract NAS 5-98033.
The author(s) of this abstract have provided an email address for comments about the abstract: ayshih@ssl.berkeley.edu
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Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.