Search for Long-Lived Radioactivity From Solar Flares With RHESSI

Details Search for Long-Lived Radioactivity From Solar Flares With RHESSI Search for Long-Lived Radioactivity From Solar Flares With RHESSI

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh43b1527s&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH43B-1527

Physics

7507 Chromosphere, 7514 Energetic Particles (2114), 7519 Flares, 7529 Photosphere, 7554 X-Rays, Gamma Rays, And Neutrinos

Scientific paper

Ions accelerated in solar flares interact with the ambient atmosphere to produce not only the prompt gamma- ray line emission that has been observed in many flares, but also radioactive nuclei with long half-lives. The most notable of these nuclei is Co-56, which has a half-life of 78.8~days and upon decay produces very narrow lines at 847~keV and 1.238~MeV. Due to the long half-life of Co-56, the radioactive material will accumulate over multiple flares and persist over many weeks. The initial fluxes seen in these lines can constrain models of ion acceleration in flares in a similar way to fluxes of the prompt lines. More importantly, their decay profile with time would provide an absolutely new probe -- a radioactive tracer -- of the mixing of material from the chromosphere and upper photosphere to greater depths. The high-resolution spectral capabilities of the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) provide the best opportunity to date for detecting such lines above the background. We present the results from our preliminary search for the lines from these long-lived radioactive nuclei. The work at the University of California, Berkeley, was supported by NASA grant NNG05GI89G.

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