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Title:
WZ Cephei: A Close Binary at the Beginning of Contact Phase
Authors:
Zhu, L. Y.; Qian, S. B.
Affiliation:
AA(National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China ; Laboratory for the Structure and Evolution of Celestial Bodies, Chinese Academy of Sciences P.O. Box 110, 650011 Kunming, China; ), AB(National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China ; Laboratory for the Structure and Evolution of Celestial Bodies, Chinese Academy of Sciences P.O. Box 110, 650011 Kunming, China)
Publication:
The Astronomical Journal, Volume 138, Issue 6, pp. 2002-2006 (2009). (AJ Homepage)
Publication Date:
12/2009
Origin:
IOP
AJ Keywords:
binaries: close, binaries: eclipsing, stars: evolution, stars: individual: WZ Cephei
DOI:
10.1088/0004-6256/138/6/2002
Bibliographic Code:
2009AJ....138.2002Z

Abstract

Photometric photoelectric data of the short-period close binary system, WZ Cephei, are presented. A new photometric analysis with the 2003 version of the Wilson-Devinney method confirmed that it is a shallow contact binary (f ~ 13.3%) with a high level of spot activity on the primary component. Combining new determined times of light minimum with the others published in the literature, the period change of the binary star is investigated. A periodic variation, with a period of 34.2 years and an amplitude of 0fd013, was discovered to be superimposed on a long-term period decrease (dP/dt = –8.8 × 10–8 days year–1). Both the secular period decrease and the shallow contact configuration suggest that this binary system is at the beginning of contact phase. It is on the way to evolving into a normal overcontact phase via secular angular momentum loss and/or mass transfer from the more massive component to the less massive one. The period oscillation can be explained either by the light-time effect due to the presence of a third body or by magnetic activity. On the one hand, if it is caused by the light-time effect, the mass and the orbital radius of the additional body should be m 3 = 0.17 M sun and a 3 = 26.6 AU, respectively, when this body is coplanar to the orbit of the eclipsing pair. On the other hand, since the system shows high levels of spot activity, the period oscillation may be explained as a consequence of magnetic cycles. In this case, the required variation of the quadrupole moment is calculated to be 9.2 × 1049 g cm2.
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