| 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 |
|