Application of the solar plasma density investigation method based on the solar flare 2.223 MeV gamma-line time profile analysis to the experimental data

Details Application of the solar plasma density investigation method based on the solar flare 2.223 MeV gamma-line time profile analysis to the experimental data Application of the solar plasma density investigation method based on the solar flare 2.223 MeV gamma-line time profile analysis to the experimental data

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....8.3060k&link_type=abstract

Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int

Physics

Scientific paper

In the previous works we have shown the possibility of determining solar plasma density altitude profile in the period of solar flare by means of solar flare 2.22 MeV neutron capture gamma-line time profile analysis. The method is a unique possibility to experimentally investigate the deep layers photospheric and subphotospheric, inaxessible to another methods. It have been shown that the most important factors, which impact on the 2.22 MeV gamma-line time profile, are characteristics of initial neutron flux, surrounding medium parameters, neutron decay, neutron and gamma-ray interactions with the medium. Previously we have made allowance for the most part of these factors. In the present work we present the exact calculaions of non-radiative absorption of neutrons by helium-3, as an additional loss of neutrons, which form 2.22 MeV gamma-emission, and investigate the solar flare gamma-line 2.22 MeV time profile dependencies on initial neutron escape geometry. Then we apply the new calculated time profiles to the analysis of the solar gamma-flares experimental data within the framework of the method.

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