High-speed photometry of the pre-cataclysmic binary HW Virginis and its orbital period change

Details High-speed photometry of the pre-cataclysmic binary HW Virginis and its orbital period change High-speed photometry of the pre-cataclysmic binary HW Virginis and its orbital period change

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...414.1043i&link_type=abstract

Astronomy and Astrophysics, v.414, p.1043-1048 (2004)

Astronomy and Astrophysics

Astrophysics

5

Stars: Individual: Hw Vir, Stars: Binaries: Eclipsing, Techniques: Photometry

Scientific paper

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 M&sun; for a hydrogen burning star. Its minimum mass is about 0.022 M&sun; and for a wide range of inclinations of third-body orbit, i.e. i ≥19o, the mass is smaller than 0.07 M&sun;. 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.

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