Study of the 28 October 2003 and 20 January 2005 solar flares by means of 2.223 MeV gamma-emission line |
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| Authors: | Evgenia V Troitskaia Irene V Arkhangelskaja Leonty I Miroshnichenko Andrey I Arkhangelsky |
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| Institution: | 1. Skobeltsyn Institute of Nuclear Physics of Moscow State University, 1(2), Leninskie Gory, GSP-1, Moscow 119991, Russia;2. Astrophysics Institute of Moscow Engineering Physics Institute (State University), Kashirskoe Shosse, 31, Moscow 115409, Russia;3. Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, RAS, IZMIRAN, 142190, Troitsk, Moscow Region, Russia;4. Instituto de Geofísica, UNAM, C.U., Coyoacán 04510, México, DF, Mexico |
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| Abstract: | By the data on intensity-time profiles of the neutron capture line of 2.223 MeV we have studied some characteristics of two solar flares, 28 October 2003 and 20 January 2005 (INTEGRAL and CORONAS-F observations, respectively). The SINP code was applied making allowance for the main processes of neutron interactions and deceleration in the solar plasma, character of neutron source, losses of neutrons and density model of the solar atmosphere. Comparison of the computed time profiles of 2.223 MeV line with observed ones for the flare of 28 October 2003 confirms the results obtained earlier for three other flares. Namely, the effect of density enhancement (EDE) in the sub-flare region, as well as the variations (hardening) of accelerated particle spectrum in the course of the event have been confirmed. The usual modeling procedure by the SINP code, however, seems to be inapplicable to the event of 20 January 2005. Possible causes of density enhancements during some flares and peculiarities of the 20 January 2005 flare are discussed. |
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| Keywords: | Particle acceleration Solar flares Neutron capture line Solar plasma density |
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