High-Resolution Observation of the Solar Positron-Electron Annihilation Line

Details High-Resolution Observation of the Solar Positron-Electron Annihilation Line High-Resolution Observation of the Solar Positron-Electron Annihilation Line

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...595l..85s&link_type=abstract

The Astrophysical Journal, Volume 595, Issue 2, pp. L85-L88.

Astronomy and Astrophysics

Astronomy

18

Sun: Flares, Sun: Particle Emission, Sun: X-Rays, Gamma Rays

Scientific paper

The Reuven Ramaty High Energy Solar Spectroscopic Imager (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 annihilation in two vastly different solar environments. It can be produced by 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 fitted by a thermal Gaussian having a width of 8.1+/-1.1 keV (FWHM), indicating temperatures of ~(4-7)×105 K. The measured 3γ/2γ ratio does not constrain the density when the annihilation takes place in such an ionized medium, although the density must be high enough to slow down the positrons. This would require the formation of a substantial mass of atmosphere at transition-region temperatures during the flare.

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