HS 1857+5144: a hot and young pre-catalysmic variable
Aungwerojwit, A. (Amornrat), Gaensicke, B. T. (Boris T.), Rodriguez-Gil, P., Hagen, H.-J., Giannakis, O., Papadimitriou, C., Prieto, C. Allende and Engels, D.. (2007) HS 1857+5144: a hot and young pre-catalysmic variable. Astronomy & Astrophysics, Vol.469 (No.1). pp. 297-305. ISSN 0004-6361Full text not available from this repository.
Official URL: http://dx.doi.org/10.1051/0004-6361:20077276
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 P-orb = 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 M-wd similar or equal to 0.6-1.0 M-circle dot and T-wd similar or equal to 70 000-100 000 K, respectively. The detection of He II lambda.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 M-sec similar or equal to 0.15-0.30 M-circle dot and i similar or equal to 45 degrees-55 degrees, 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 similar to 10(5) yr ago. HS 1857+5144 will start mass transfer within or below the 2-3 h period gap.
|Item Type:||Journal Article|
|Subjects:||Q Science > QB Astronomy|
|Divisions:||Faculty of Science > Physics|
|Journal or Publication Title:||Astronomy & Astrophysics|
|Official Date:||July 2007|
|Number of Pages:||9|
|Page Range:||pp. 297-305|
|Access rights to Published version:||Restricted or Subscription Access|
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