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On the formation of Mg II h and k lines in solar prominences
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SYSNO ASEP 0429300 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title On the formation of Mg II h and k lines in solar prominences Author(s) Heinzel, Petr (ASU-R) RID, ORCID
Vial, J. C. (FR)
Anzer, U. (DE)Source Title Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 564, April (2014), A132/1-A132/10Number of pages 10 s. Publication form Print - P Language eng - English Country FR - France Keywords line: profiles ; line: formation ; Sun: filaments, prominences Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics R&D Projects GAP209/12/0906 GA ČR - Czech Science Foundation (CSF) GAP209/11/2463 GA ČR - Czech Science Foundation (CSF) GA205/09/1705 GA ČR - Czech Science Foundation (CSF) Institutional support ASU-R - RVO:67985815 UT WOS 000334671000132 DOI 10.1051/0004-6361/201322886 Annotation We computed the Mg II h and k line profiles that are emergent from prominence-slab models and show their dependence on kinetic temperature, gas pressure, geometrical extension, and microturbulent velocity. By increasing the line opacity, significant departures from the complete frequency redistribution take place in the line wings. Models with a PCTR temperature structure show that Mg II becomes ionized to Mg III in the temperature range between roughly 15 000 and 30 000 K. Doppler dimming is significant for Mg II resonance lines. At the velocity 300 km s(-1), the line intensity decreases to about 20% of the value for static prominences. Finally, we demonstrate the role of Mg II h and k radiation losses on the prominence energy balance. Their dominant role is at lower pressures, while the losses due to hydrogen and Can dominate at higher pressures. Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2015
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