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Title:
High-speed photometry of the pre-cataclysmic binary HW Virginis and its orbital period change
Authors:
İbanoǧlu, C.; Çakırlı, Ö.; Taş, G.; Evren, S.
Affiliation:
AA(Ege University Observatory, 35100 Bornova, İzmir, Turkey), AB(Ege University Observatory, 35100 Bornova, İzmir, Turkey), AC(Ege University Observatory, 35100 Bornova, İzmir, Turkey), AD(Ege University Observatory, 35100 Bornova, İzmir, Turkey)
Publication:
Astronomy and Astrophysics, v.414, p.1043-1048 (2004) (A&A Homepage)
Publication Date:
02/2004
Origin:
A&A
A&A Keywords:
stars: individual: HW Vir, stars: binaries: eclipsing, techniques: photometry
DOI:
10.1051/0004-6361:20034013
Bibliographic Code:
2004A&A...414.1043I

Abstract

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