Volume 469, Number 1, July I 2007
|Page(s)||297 - 305|
|Section||Stellar structure and evolution|
|Published online||24 April 2007|
HS 1857+5144: a hot and young pre-cataclysmic variable
Department of Physics, University of Warwick, Coventry, CV4 7AL, UK e-mail: A.Aungwerojwit@warwick.ac.uk
2 Department of Physics, Faculty of Science, Naresuan University, Phitsanulok 65000, Thailand
3 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
4 Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
5 Institute of Astronomy and Astrophysics, National Observatory of Athens, PO Box 20048, Athens 11810, Greece
6 McDonald Observatory and Department of Astronomy, University of Texas, Austin, TX 78712, USA
Accepted: 11 April 2007
Aims.We report the discovery of a new white dwarf/M dwarf binary, HS 1857+5144, identified in the Hamburg Quasar Survey (HQS).
Methods.Time-resolved optical spectroscopy and photometry were carried out to determine the properties of this new cataclysmic variable progenitor (pre-CV).
Results.The light curves of HS 1857+5144 display a sinusoidal variation with a period of Porb = 383.52 min and peak-to-peak amplitudes of 0.7 mag and 1.1 mag in the B-band and R-band, respectively. The large amplitude of the brightness variation results from a reflection effect on the heated inner hemisphere of the companion star, suggesting a very high temperature of the white dwarf. Our radial velocity study confirms the photometric period as the orbital period of the system. A model atmosphere fit to the spectrum of the white dwarf obtained at minimum light provides limits to its mass and temperature of 0.6-1.0 and 70 000-100 000 K, respectively. The detection of 4686 absorption classifies the primary star of HS 1857+5144 as a DAO white dwarf. Combining the results from our spectroscopy and photometry, we estimate the mass of the companion star and the binary inclination to be 0.15-0.30 and 45°-55°, respectively.
Conclusions.We classify HS 1857+5144 as one of the youngest pre-CV known to date. The cooling age of the white dwarf suggests that the present system has just emerged from a common envelope phase ~105 yr ago. HS 1857+5144 will start mass transfer within or below the 2–3 h period gap.
Key words: stars: binaries: close / stars: individual: HS 1857+5144
© ESO, 2007
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