Relative timing of solar prompt γ-ray line and X-ray emission produced by flare accelerated ions and electrons

Details Relative timing of solar prompt γ-ray line and X-ray emission produced by flare accelerated ions and electrons Relative timing of solar prompt γ-ray line and X-ray emission produced by flare accelerated ions and electrons

Sep 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988aipc..170..252h&link_type=abstract

AIP Conference Proceedings, Volume 170, pp. 252-257 (1988).

Physics

1

X-Ray

Scientific paper

SMM and Hinotori observations show that the peak time of the γ-ray emission is sometimes delayed with respect to the one of the hard X-ray flux. Such delays may be interpreted either as an evidence of a two step acceleration process of electrons and ions or as the result of the partial trapping and/or propagation of the particles from the acceleration region to the interaction site. Here we focus on the latter hypothesis and present some preliminary calculations of the time dependent transport of energetic ions. Preliminary estimates of the 4.4 MeV line emission are used to discuss the relative timing of Hard X-ray and γ-ray emissions. One difficulty with the preliminary model discussed here is that the number of ions involved in the γ-ray line production is very large. Nevertheless, for reasonable parameters, a good agreement is found between observed and expected delays.

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