On Period Variations of the K-Type Eclipsing Binary BM Ursae Majoris

Details On Period Variations of the K-Type Eclipsing Binary BM Ursae Majoris On Period Variations of the K-Type Eclipsing Binary BM Ursae Majoris

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009pasj...61...13y&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.61, No.1, pp.13--18

Astronomy and Astrophysics

Astronomy

4

Stars: Binaries: Close, Stars: Binaries: Eclipsing, Stars: Individual (Bm Urase Majoris)

Scientific paper

From new CCD observations, 11 light minimum times are presented in this paper. The orbital period change of a W UMa-type eclipsing binary, BM Urase Majoris, was investigated, based on all available times of light minimum. It was discovered that the orbital period of the binary shows cyclic oscillation, superimposed on a secular period decrease. The amplitude and the period of the cyclic variation are A = 0.0101(±0.0004)d and P3 = 30.8(±0.2)yr, respectively. This kind of cyclic variation may be due to a light-time effect via an unseen third body. If the existence of an additional body is true, it may remove a great amount of angular momentum from the central system, and may play an important role in the formation of close binary. The orbital period continuously decreases at a rate of dP/dt = -7.49(±0.16) × 10-8d yr-1, which may be due to mass transfer from the primary to the secondary, accompanying mass and angular-momentum loss from the binary system. The orbital period decrease, accompanying mass and angular momentum loss, would cause the contact degree to increase. Therefore, this binary will evolve into a deep contact configuration.

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