Temporal Variability of Gamma-Ray Lines from the X-Class Solar Flare of 2002 July 23

Details Temporal Variability of Gamma-Ray Lines from the X-Class Solar Flare of 2002 July 23 Temporal Variability of Gamma-Ray Lines from the X-Class Solar Flare of 2002 July 23

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh11d1132s&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH11D-1132

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7514 Energetic Particles (2114), 7519 Flares, 7529 Photosphere, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

On 2002 July 23, the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) detected a GOES X4.8 solar flare, and analysis of the data has produced the first spectrally resolved measurement of nuclear de-excitation gamma-ray lines in a solar flare. These narrow lines result from accelerated ions colliding with the ambient medium (which includes Fe, Mg, Ne, Si, C, and O nuclei), and thus their relative fluxes probe the composition of the solar atmosphere. We investigate the temporal variability of the flux of these lines by analyzing the observed spectrum for two separate time intervals of the flare (00:27:20-00:32:56 UT and 00:32:56-00:43:20 UT). The relative fluxes in the gamma-ray lines change dramatically between these two intervals, suggesting that the circumstances of ion acceleration change as the flare progresses. We consider the possibility of variations in the nuclear abundances, as well as other possible causes such as a varying alpha/proton ratio or a varying energy spectrum for the accelerated ions. Finally, we compare these variations with the source locations as determined by RHESSI's gamma-ray imaging. The work at the University of California, Berkeley, was supported by NASA contract NAS 5-98033.

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