dc.contributor.author |
Anupama, G. C |
|
dc.contributor.author |
Prabhu, T. P |
|
dc.date.accessioned |
2011-03-14T10:25:44Z |
|
dc.date.available |
2011-03-14T10:25:44Z |
|
dc.date.issued |
1993 |
|
dc.identifier.citation |
Regev, O & Shaviv, G., Cataclysmic Variables and related physics, 2nd technion Haifa conference, p. 271 |
en |
dc.identifier.uri |
http://hdl.handle.net/2248/5416 |
|
dc.description.abstract |
Spectroscopy of the ONeMg nova Cygni 1992 is presented, based on data obtained
at the Vainu Bappu Observatory between 1992 March l3-May 22 and
1993 January 3. Spectra were obtained at five epochs- epoch I: 1992 March
13-14, 20 days after the outburst maximum; epoch II: 1992 March 22-24, 30
days after maximum; epoch III: 1992 April 20, 58 days after maximum; epoch
IV: 1992 May 21-22, 90 days after maximum; and epoch V: 1993 January 3, 347
days after maximum. The spectrum during epochs I-II is dominated by strong
broad P -Cygni emission lines predominantly of hydrogen Balmer and Fe II lines.
Lines due to N II, Mg II and He I are also strong. [OI] auroral and nebular lines
are also present. In the red region of the spectrum, 0 17774,8446 and lines due
to Mg II, N I and Ca II are strong, with the strength of 0 I 8446 line indicating
Lyf3 fluorescence and a high optical depth. Epochs III-V show It steady increase
in the strength of He I and [O III] lines, while the strength of the other permitted
lines steadily decreases. On day 347, [O III] 4959+5007 is 3 times stronger than
Halpha and 8 times stronger than Hp. |
en |
dc.language.iso |
en |
en |
dc.publisher |
Institute of Physics Publishing |
en |
dc.relation.ispartofseries |
Annals of the Israel Physical Society, Vol. 10 |
|
dc.title |
The Optical Spectrum of Nova Cygni 1992 |
en |
dc.type |
Article |
en |