RHESSI Observation of the Solar Annihilation Line

Details RHESSI Observation of the Solar Annihilation Line RHESSI Observation of the Solar Annihilation Line

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....6.3199s&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

Scientific paper

RHESSI has observed the positron-electron annihilation line at 511 keV produced during the 2002 July 23 solar flare. The shape of the line is consistent with formation of positronium by charge exchange in flight with hydrogen in a quiet solar atmosphere at a temperature of ˜ 6000 K. However, the measured upper limit to the 3γ /2γ ratio (ratio of annihilation photons in the positronium continuum to the number in the line) is only marginally consistent with what is calculated for this environment. The annihilation line can also be fit by a thermal Gaussian having a width of 8.1 ± 1.1 keV (FWHM), indicating temperatures of ˜ 4 - 7 × 105 K. This would require the formation of a substantial mass of atmosphere at transition-region temperatures during the flare.

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