Počet záznamů: 1
On the formation of Mg II h and k lines in solar prominences
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SYSNO ASEP 0429300 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název On the formation of Mg II h and k lines in solar prominences Tvůrce(i) Heinzel, Petr (ASU-R) RID, ORCID
Vial, J. C. (FR)
Anzer, U. (DE)Zdroj.dok. Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 564, April (2014), A132/1-A132/10Poč.str. 10 s. Forma vydání Tištěná - P Jazyk dok. eng - angličtina Země vyd. FR - Francie Klíč. slova line: profiles ; line: formation ; Sun: filaments, prominences Vědní obor RIV BN - Astronomie a nebeská mechanika, astrofyzika CEP GAP209/12/0906 GA ČR - Grantová agentura ČR GAP209/11/2463 GA ČR - Grantová agentura ČR GA205/09/1705 GA ČR - Grantová agentura ČR Institucionální podpora ASU-R - RVO:67985815 UT WOS 000334671000132 DOI 10.1051/0004-6361/201322886 Anotace 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. Pracoviště Astronomický ústav Kontakt Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2015
Počet záznamů: 1