Volume 414, Number 3, February II 2004
|Page(s)||1043 - 1048|
|Section||Stellar structure and evolution|
|Published online||27 January 2004|
High-speed photometry of the pre-cataclysmic binary HW Virginis and its orbital period change
Ege University Observatory, 35100 Bornova, İzmir, Turkey
Corresponding author: C. İbanoǧlu, firstname.lastname@example.org
Accepted: 8 August 2003
The broad band B and V light curves of the pre-cataclysmic eclipsing binary HW Vir were obtained. All the available eclipse timings, including the new ones, spanning 19 years were analyzed under the third-body hypothesis. The residuals between the observed and calculated times of mid-eclipse show a long-term sinusoidal variation. The analysis yields the parameters of the third-body orbit, as well as limiting mass for the tertiary object. The result of this analysis gives a light-time semi-amplitude of 112 s, an orbital period of 18.8 yr and an eccentricity of 0.12. The mass of the third star is below the theoretical threshold of 0.07 for a hydrogen burning star. Its minimum mass is about 0.022 and for a wide range of inclinations of third-body orbit, i.e. , the mass is smaller than 0.07 . Therefore, we suggest that the third star may be a brown dwarf candidate. Combining the semi-amplitudes of the radial velocities and the photometric light curve solution has allowed us to model the short-period detached binary HW Vir. The luminosity and radius of the dM companion are slightly larger than that given by low-mass models.
Key words: stars: individual: HW Vir / stars: binaries: eclipsing / techniques: photometry
© ESO, 2004
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