Orbital Period Variation and Morphological Light Curve Studies for the W UMa Binary BB Pegasi

Details Orbital Period Variation and Morphological Light Curve Studies for the W UMa Binary BB Pegasi Orbital Period Variation and Morphological Light Curve Studies for the W UMa Binary BB Pegasi

Jun 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011jkas...44...97h&link_type=abstract

Journal of the Korean Astronomical Society, vol. 44, no. 3, pp. 97-108

Astronomy and Astrophysics

Astronomy

Binaries: Close, Binaries: Eclipsing, Stars: Individual (Bb Peg), Stars: W, Subtype W Uma, Period Variation: Magnetic Activity

Scientific paper

The photometric light curves of the W-type W UMa eclipsing contact binary system BB Pegasi have been found to be extremely asymmetric over all the observed 63 years in all wavelengths UBVR. The light curves have been characterized by occultation primary minima. So, the morphology of these light curves has been studied in view of these different asymmetric degrees. The system shows a distinct O'Connell effect as well as depth variation. A 22.96 years cycle, of dark spots group, has been determined for the system combined with about the same cycling for the depth variations (22.78 yr). Also, an analysis of the measurements of mid-eclipse times of BB Peg has been presented. The analysis indicates a period decrease of 5.62× 10-8 d/yr, which can be interpreted in terms of mass transfer of rate -4.38 × 10-8 M_&sun;/yr, from the more to the less massive component. The O-C diagram shows a damping sine wave covering two different cycles of 17.0 yr and 12.87 yr with amplitudes equal to 0.0071 and 0.0013 day, respectively. These unequal durations show a non periodicity which may be explained as a result of magnetic activity cycling variations due to star spots. The obtained characteristics are consistent when applying Applegate's (1992) mechanism.

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