| Issue |
A&A
Volume 367, Number 2, February IV 2001
|
|
|---|---|---|
| Page(s) | 588 - 596 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361:20000446 | |
| Published online | 15 February 2001 | |
The dwarf nova binary system BV Puppis
1
Dept. of Physics and Astronomy, University of Wyoming, PO Box 3905, Laramie, WY 82071, USA
2
On leave from Dipartimento Di Astronomia, dell'Universitá di Padova, Italy
3
University of St-Andrews, School of Physics and Astronomy, North Haugh, St Andrews, Fife, KY16-9SS, Scotland
4
On leave from Campbell County High School, 1000 Camel Dr., Gillette, WY 82716, USA
5
Astrophysics Group, Planetary Science Institute, 620 N. 6th Ave., Tucson, AZ 85705, USA
Corresponding author: A. Bianchini, bianchini@pd.astro.it
Received:
5
October
2000
Accepted:
4
November
2000
Medium resolution spectra of the dwarf nova BV Pup obtained during an outburst confirm the relatively long orbital period
(
h). The emission lines reveal rather structured profiles that are produced
in the disc and in the stream. Doppler tomography shows clear bright spot regions in Hβ
and HeII 4686 Åemission line flux. Dynamical solutions for the system parameters are only
found if the external radius of the accretion disc is close to the circularisation radius.
The white dwarf mass is 
, the orbital inclination 
.
Key words: stars: individual BV Pup / stars: dwarf novae, cataclysmic variables
© ESO, 2001
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