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Shock-reflected electrons and X-ray line spectra
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SYSNO ASEP 0478684 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Shock-reflected electrons and X-ray line spectra Author(s) Dzifčáková, Elena (ASU-R) RID, ORCID
Vandas, Marek (ASU-R) RID, ORCID
Karlický, Marian (ASU-R) RID, ORCIDSource Title Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 603, July (2017), A17/1-A17/8Number of pages 8 s. Publication form Online - E Language eng - English Country FR - France Keywords Sun ; flares ; line formation Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics OECD category Astronomy (including astrophysics,space science) R&D Projects GA17-16447S GA ČR - Czech Science Foundation (CSF) GAP209/12/0103 GA ČR - Czech Science Foundation (CSF) GA14-19376S GA ČR - Czech Science Foundation (CSF) GA17-06065S GA ČR - Czech Science Foundation (CSF) GA15-17490S GA ČR - Czech Science Foundation (CSF) GA16-13277S GA ČR - Czech Science Foundation (CSF) Institutional support ASU-R - RVO:67985815 UT WOS 000406619100075 EID SCOPUS 85021699068 DOI 10.1051/0004-6361/201630306 Annotation 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.
Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2018
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