Radiative transfer in the co-moving frame

dc.contributor.author	Peraiah, A
dc.date.accessioned	2009-01-02T11:21:27Z
dc.date.available	2009-01-02T11:21:27Z
dc.date.issued	1981-06
dc.identifier.citation	Astrophysics and Space Science, Vol. 77, No. 1, pp. 243 - 255	en
dc.identifier.issn	0004-640X
dc.identifier.uri	http://hdl.handle.net/2248/4235
dc.description.abstract	Solution of line-transfer equation in the co-moving frame, obtained on the basis of discrete space theory, has been employed to calculate the lines emerging from a rapidly expanding stellar atmosphere. The solution is found to be highly stable for large velocities of expansion with both positive and negative velocity gradients. Profiles of spectral lines have been presented that are translated along the line of sight of the observer at infinity. A non-LTE two-level atom has been treated in a medium scattering isotropically with line and continuum emission P Cygni-type profiles noticed in a purely scattering medium.	en
dc.language.iso	en	en
dc.publisher	D. Reidel Publishing Co.	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1981Ap%26SS..77..243P	en
dc.relation.uri	http://www.springerlink.com/content/wh36676257593x14/	en
dc.rights	© D. Reidel Publishing Co.	en
dc.subject	Gas Expansion	en
dc.subject	Radiative Transfer	en
dc.subject	Stellar Atmospheres	en
dc.subject	Stellar Spectra	en
dc.subject	Continuous Spectra	en
dc.subject	Line Spectra	en
dc.subject	Nonequilibrium Conditions	en
dc.subject	Stellar Mass Ejection	en
dc.title	Radiative transfer in the co-moving frame	en
dc.type	Article	en