Volume 504, Number 2, September III 2009
|Page(s)||491 - 499|
|Section||Stellar structure and evolution|
|Published online||15 July 2009|
Observations of three pre-cataclysmic variables from the Edinburgh-Cape blue object survey
Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica, Vicuña Mackenna 4860, 782-0436 Macul, Chile e-mail: email@example.com,firstname.lastname@example.org,email@example.com
2 Department of Physics, University of Warwick, Coventry CV4 7AL, UK e-mail: [Boris.Gaensicke;j.k.taylor]@warwick.ac.uk
3 Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium e-mail: firstname.lastname@example.org
4 Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile e-mail: email@example.com
Accepted: 20 May 2009
Aims. This study aims at determining the parameters of the three candidate pre-cataclysmic binaries EC 12477–1738, EC 13349–3237, and EC 14329–1625, most importantly their orbital period.
Methods. Time-series photometry reveals orbital modulation in the form of sinusoidal variation due to the reflection effect. Photometric observations are complemented by time-resolved spectroscopy that yields radial velocities of the Hα emission line. The combination of both methods allows us to unambiguously determine the orbital periods. The average spectra are used to estimate physical parameters of the primary and secondary stellar components.
Results. We determine the orbital period for EC 12477–1738 as 0.362 d, thus confirming the value previously reported. A similar period, d, is found for EC 14329–1625. Both systems incorporate a medium-hot white dwarf ( K) and an M3V secondary star. The third pre-CV, EC 13349–3237, is the youngest of the three, with a hot WD ( K), and it also has the longest period d. It furthermore turns out to be one of the still rare pre-CVs with a comparatively early-type, M1V, secondary star, which will eventually evolve into a CV above the period gap.
Key words: binaries: close / stars: late-type / white dwarfs / novae, cataclysmic variables
© ESO, 2009
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