Shock-reflected electrons and X-ray line spectra

0478684 - ASÚ 2018 RIV FR eng J - Journal Article
Dzifčáková, Elena - Vandas, Marek - Karlický, Marian
Shock-reflected electrons and X-ray line spectra.
Astronomy & Astrophysics. Roč. 603, July (2017), A17/1-A17/8. ISSN 0004-6361. E-ISSN 1432-0746
R&D Projects: GA ČR(CZ) GA17-16447S; GA ČR GAP209/12/0103; GA ČR(CZ) GA14-19376S; GA ČR(CZ) GA17-06065S; GA ČR GA15-17490S; GA ČR(CZ) GA16-13277S
Institutional support: RVO:67985815
Keywords : Sun * flares * line formation
OECD category: Astronomy (including astrophysics,space science)
Impact factor: 5.565, year: 2017

The aim of this paper is to try to explain the physical origin of the non-thermal electron distribution that is able to form the enhanced intensities of satellite lines in the X-ray line spectra observed during the impulsive phases of some solar flares. Synthetic X-ray line spectra of the distributions composed of the distribution of shock reflected electrons and the background Maxwellian distribution are calculated in the approximation of non-Maxwellian ionization, recombination, excitation and de-excitation rates. The distribution of shock reflected electrons is determined analytically. We found that the distribution of electrons reflected at the nearly-perpendicular shock resembles, at its high-energy part, the so called n-distribution. Therefore it could be able to explain the enhanced intensities of Si XIId satellite lines. However, in the region immediately in front of the shock its effect is small because electrons in background Maxwellian plasma are much more numerous there.

Permanent Link: http://hdl.handle.net/11104/0274744