On some visible and infrared atomic hydrogen lines in three photospheric models

dc.contributor.author	Bondal, K. R.
dc.contributor.author	Gaur, V. P.
dc.date.accessioned	2010-02-16T09:37:22Z
dc.date.available	2010-02-16T09:37:22Z
dc.date.issued	1986
dc.identifier.uri	http://hdl.handle.net/123456789/525
dc.description.abstract	The behavior of the line profiles in the wings of the first four lines of the Balmer, Paschen and Brackett series in the solar spectrum at the disc centre has been investigated with a view to comparing the computed profiles (Holweger & Muiler 1974; Vernazza, Avrett & Loeser 1976, 1981) with observations. The comparison shows that, in general, the HOlweger & Muller model can explain the lines of Balmer series better than the lines of Paschen and of Brackett series. The reverse is the case with the Vernazza, Avrett & Loeser Models.	en_US
dc.language.iso	en	en_US
dc.relation.ispartofseries	basi14-73
dc.subject	Hydrogen Lines, Photospheric Models, Stark-broadening	en_US
dc.title	On some visible and infrared atomic hydrogen lines in three photospheric models	en_US
dc.type	Article	en_US