EDP Sciences
Free access
Issue
A&A
Volume 367, Number 2, February IV 2001
Page(s) 588 - 596
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20000446


A&A 367, 588-596 (2001)
DOI: 10.1051/0004-6361:20000446

The dwarf nova binary system BV Puppis

A. Bianchini1, 2, W. Skidmore3, 1, J. M. Bailey1, 4, S. Howell5, 1 and R. Canterna1

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

(Received 5 October 2000 / Accepted 4 November 2000)

Abstract
Medium resolution spectra of the dwarf nova BV Pup obtained during an outburst confirm the relatively long orbital period ($P \sim6.4$ 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 H$\beta$ 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 $1.2 \pm 0.2 M_{\odot}$, the orbital inclination $23^\circ \pm 3^\circ$.


Key words: stars: individual BV Pup -- stars: dwarf novae, cataclysmic variables

Offprint request: A. Bianchini, bianchini@pd.astro.it

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© ESO 2001