Deep, Low-mass Ratio Overcontact Binary Systems. XII. CK Bootis with Possible Cyclic Magnetic Activity and Additional Companion

Details Deep, Low-mass Ratio Overcontact Binary Systems. XII. CK Bootis with Possible Cyclic Magnetic Activity and Additional Companion Deep, Low-mass Ratio Overcontact Binary Systems. XII. CK Bootis with Possible Cyclic Magnetic Activity and Additional Companion

May 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aj....143..122y&link_type=abstract

The Astronomical Journal, Volume 143, Issue 5, article id. 122 (2012).

Astronomy and Astrophysics

Astronomy

Binaries: Close, Binaries: Eclipsing, Stars: Individual: Ck Bootis

Scientific paper

We present precision CCD photometry, a period study, and a two-color simultaneous Wilson code solution of the short-period contact binary CK Bootis. The asymmetric light curves were modeled by a dark spot on the primary component. The result identifies that CK Boo is an A-type W UMa binary with a high fillout of f = 71.7(± 4.4)%. From the O – C curve, it is found that the orbital period changes in a complicated mode, i.e., a long-term increase with two sinusoidal variations. One cyclic oscillation with a period of 10.67(± 0.20) yr may result from magnetic activity cycles, which are identified by the variability of Max. I – Max. II. Another sinusoidal variation (i.e., A = 0.0131 days(± 0.0009 days) and P 3 = 24.16(± 0.64) yr) may be attributed to the light-time effect due to a third body. This kind of additional companion can extract angular momentum from the central binary system. The orbital period secularly increases at a rate of dP/dt = +9.79 (±0.80) × 10‑8 days yr‑1, which may be interpreted by conservative mass transfer from the secondary to the primary. This kind of deep, low-mass ratio overcontact binaries may evolve into a rapid-rotating single star, only if the contact configuration do not break down at J spin > (1/3)J orb.

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