On estimation of the optical thickness in solar prominences

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On estimation of the optical thickness in solar prominences

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dc.contributor.author Milić, Ivan
dc.contributor.author Dejanić, Sanda
dc.contributor.author Kotrč, Pavel
dc.contributor.editor Kovačević, Andjelka
dc.date.accessioned 2011-01-25T10:08:56Z
dc.date.available 2011-01-25T10:08:56Z
dc.date.issued 2008
dc.identifier.isbn 978-86-80019-30-7 en_US
dc.identifier.uri http://hdl.handle.net/123456789/1556
dc.description.provenance Submitted by Slavisha Milisavljevic (slavisha) on 2011-01-25T10:08:56Z No. of bitstreams: 1 Milic.pdf: 554551 bytes, checksum: 920f7ac81f2f8c531a530962e587fbc5 (MD5) en
dc.description.provenance Made available in DSpace on 2011-01-25T10:08:56Z (GMT). No. of bitstreams: 1 Milic.pdf: 554551 bytes, checksum: 920f7ac81f2f8c531a530962e587fbc5 (MD5) Previous issue date: 2008 en
dc.language.iso en en_US
dc.publisher Astronomical Observatory Belgrade en_US
dc.title On estimation of the optical thickness in solar prominences en_US
mf.subject.keywords Here we present a method for estimating the optical thickness of prominences from H® emission line pro¯les. The method is based on ¯tting the pro¯le with a theoretically derived function of optical thickness and value of source function. The method is applied on 52 prominences observed in Ondrejov, CR from April 2007. to March 2008. Results have been compared with the values of the optical thickness derived by other methods (by using integral intensity of H® emission line, and by numerical modeling). en_US
mf.document.pages 12 en_US
mf.contributor.editor-in-chief Dimitrijević, S. Milan
mf.contributor.technical-editor Milovanov, Tatjana

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