AAS 195th Meeting, January 2000
Session 36. White Dwarfs New and Old
Display, Thursday, January 13, 2000, 9:20am-6:30pm, Grand Hall

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[36.04] Spectroscopic Observations of the Dwarf Nova BV Puppis

J.M. Bailey (Campbell Co. H.S. / W.I.R.O.), R. Canterna (U. of Wyoming), A. Bianchini (U. of Padova / W.I.R.O.), W. Skidmore (U. of St. Andrews / W.I.R.O.), S. Howell (P. S. I. / W.I.R.O.)

Medium resolution spectra of the dwarf nova BV Pup taken during outburst at La Silla (ESO) confirm the relatively long orbital period (P ~ 6.4 h) of this close binary system. The emission lines reveal rather structured profiles. We believe these are mainly produced in the stream and the optically thin regions of the disc. A possible eclipse of the stream by the secondary is observed in the H\beta emission lines. A photometric period (P ~ 5.8 h) shorter than the spectroscopic period is observed during light maximum. Doppler tomography suggests a systemic velocity of \gamma0=37.7±4.8 km s-1.

This research was supported by NSF grant AST 9732039.

The author(s) of this abstract have provided an email address for comments about the abstract: canterna@uwyo.edu

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