Issue |
A&A
Volume 384, Number 3, March IV 2002
|
|
---|---|---|
Page(s) | 982 - 986 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20020064 | |
Published online | 15 March 2002 |
Nova Cygni 2001/2 = V2275 Cyg*
1
Department of Experimental Physics and Astronomical Observatory, University of Szeged, Szeged, Dóm tér 9., 6720, Hungary
2
Department of Optics and Quantum Electronics, University of Szeged, POB 406, Szeged, 6701, Hungary
3
David Dunlap Observatory, University of Toronto, Richmond Hill, Canada
Corresponding author: L. L. Kiss, l.kiss@physx.u-szeged.hu
Received:
26
November
2001
Accepted:
11
January
2002
We present an analysis of low- and medium resolution spectra of the
very fast nova, Nova Cygni 2001/2 (V2275 Cyg) obtained at nine epochs in
August, September and October, 2001. The expansion velocity from
hydrogen Balmer lines is found to be 2100 km s-1, although
an early Hα profile showed a weak feature at -3500 km s-1, too.
The overall appearance of the optical spectrum is dominated by
broad lines of H, He and N, therefore, the
star belongs to the “He/N” subclass of novae defined
by Williams ([CITE]). Interstellar lines and bands, as well as BV photometry
taken from the literature yielded to a fairly high reddening
of . The visual light curve was used to deduce
MV by the maximum magnitude versus rate of decline
relationship. The resulting parameters are:
,
days,
days,
.
Adopting these parameters, the star lies between 3 kpc and 8 kpc from
the Sun.
Key words: stars: novae, cataclysmic variables / stars: individual: V2275 Cyg
© ESO, 2002
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