Orbital Period Changes for the Weak-Contact Binary TY Bootis

Details Orbital Period Changes for the Weak-Contact Binary TY Bootis Orbital Period Changes for the Weak-Contact Binary TY Bootis

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aj....134..179y&link_type=abstract

The Astronomical Journal, Volume 134, Issue 1, pp. 179-184.

Astronomy and Astrophysics

Astronomy

15

Binaries: Close, Binaries: Eclipsing, Stars: Evolution, Stars: Individual: Ty Bootis

Scientific paper

We present a detailed period analysis of TY Bootis, based on all available light minimum times covering about 80 years. We discovered that there exists a cyclic variation overlaying a secular period decrease from the distorted (O-C) diagram. A long-term decrease with a sinusoidal oscillation (i.e., eq. [2]) or with a light-time effect (i.e., eq. [3]) may be reasonable due to the smaller difference between their sum of residuals. The sinusoidal change with a period of 59.7 yr for equation (2) can be attributed to either a light-time effect or cyclic magnetic activity of both components. For the assumed third body, the period and eccentricity of the light-time orbit are P3=58.6 yr and e'=0.1744, respectively. If the existence of an additional unseen body is true, this binary may be a tertiary system. The long-term orbital period decrease suggests that TY Boo is undergoing a mass transfer from the primary component to the secondary component at a rate of dm/dt=-3.15×10-8 Msolar yr-1 for equation (2) or dm/dt=-2.90×10-8 Msolar yr-1 for equation (3). As its mass transfers, accompanied by angular momentum loss due to mass outflow L2, this binary will evolve into a deep contact configuration.

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