Issue |
A&A
Volume 474, Number 1, October IV 2007
|
|
---|---|---|
Page(s) | 205 - 211 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20077316 | |
Published online | 10 September 2007 |
The pre-cataclysmic variable, LTT 560
1
Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica, Vicuña Mackenna 4860, 782-0436 Macul, Chile e-mail: ctappert@astro.puc.cl
2
Department of Physics, University of Warwick, Coventry CV4 7AL, UK e-mail: [Boris.Gaensicke;a.aungwerojwit]@warwick.ac.uk
3
European Southern Observatory, Casilla 19001, Santiago 19, Chile e-mail: lschmidt@eso.org
4
Department of Physics, Faculty of Science, Naresuan University, Phitsanulok 65000, Thailand
5
Departamento de Física, Universidad de Concepción, Casilla 160-C, Concepción, Chile e-mail: rmennick@astro-udec.cl
6
Institut für Theoretische Physik und Astrophysik, University of Kiel, 24098 Kiel, Germany e-mail: koester@astrophysik.uni-kiel.de
Received:
16
February
2007
Accepted:
11
August
2007
Aims. System parameters of the object LTT 560 are determined in order to clarify its nature and evolutionary status.
Methods. We apply time-series photometry to reveal orbital modulations of the light curve, time-series spectroscopy to measure radial velocities of features from both the primary and the secondary star, and flux-calibrated spectroscopy to derive temperatures of both components.
Results.
We find that LTT 560 is composed of a low temperature (T ~ 7500 K) DA white dwarf as the primary and an M5.5±1
main-sequence star as the secondary component. The current orbital period is Porb = 3.54(07) h. We derive a mass ratio = 0.36(03) and estimate
the distance to d = 25–40 pc. Long-term variation of the orbital light curve and an additional
Hα emission component on the white dwarf indicate activity in the system, probably in the form of flaring and/or
accretion events.
Key words: binaries: close / stars: late-type / white dwarfs / novae, cataclysmic variables
© ESO, 2007
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