About: On the formation of Mg II h and k lines in solar prominences

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rdf:type	skos:Concept http://linked.opendata.cz/ontology/domain/vavai/Vysledek
Description	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. 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. (en)
Title	On the formation of Mg II h and k lines in solar prominences On the formation of Mg II h and k lines in solar prominences (en)
skos:prefLabel	On the formation of Mg II h and k lines in solar prominences On the formation of Mg II h and k lines in solar prominences (en)
skos:notation	RIV/67985815:_____/14:00429300!RIV15-GA0-67985815
http://linked.open...avai/riv/aktivita	I P
http://linked.open...avai/riv/aktivity	I, P(GA205/09/1705), P(GAP209/11/2463), P(GAP209/12/0906)
http://linked.open...iv/cisloPeriodika	April
http://linked.open...vai/riv/dodaniDat	2015
http://linked.open...aciTvurceVysledku	Heinzel, Petr
http://linked.open.../riv/druhVysledku	J - Článek v odborném periodiku
http://linked.open...iv/duvernostUdaju	S - Úplné a pravdivé údaje nepodléhající ochraně podle zvláštních právních předpisů
http://linked.open...titaPredkladatele	Astronomický ústav AV ČR, v. v. i.
http://linked.open...dnocenehoVysledku	34440
http://linked.open...ai/riv/idVysledku	RIV/67985815:_____/14:00429300
http://linked.open...riv/jazykVysledku	eng - angličtina
http://linked.open.../riv/klicovaSlova	line: profiles; line: formation; Sun: filaments, prominences (en)
http://linked.open.../riv/klicoveSlovo	Sun: filaments prominences line: formation line: profiles
http://linked.open...odStatuVydavatele	FR - Francouzská republika
http://linked.open...ontrolniKodProRIV	[F9EAB7728833]
http://linked.open...i/riv/nazevZdroje	Astronomy & Astrophysics
http://linked.open...in/vavai/riv/obor	BN
http://linked.open...ichTvurcuVysledku	1 (xsd:int)
http://linked.open...cetTvurcuVysledku	3 (xsd:int)
http://linked.open...vavai/riv/projekt	Diagnostics of the non-thermal electron distributions in the solar korona Realistic solar prominence models combining radiative transfer modeling and MHD simulatios Analysis and modeling of Ellerman bombs
http://linked.open...UplatneniVysledku	2014
http://linked.open...v/svazekPeriodika	564
http://linked.open...iv/tvurceVysledku	Heinzel, Petr Anzer, U. Vial, J. C.
http://linked.open...ain/vavai/riv/wos	000334671000132
issn	0004-6361
number of pages	10 (xsd:int)
http://bibframe.org/vocab/doi	10.1051/0004-6361/201322886

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