Simultaneous light and velocity curve solution and probable starspot activities for the W UMa system U Pegasi

Details Simultaneous light and velocity curve solution and probable starspot activities for the W UMa system U Pegasi Simultaneous light and velocity curve solution and probable starspot activities for the W UMa system U Pegasi

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ap%26ss.146....1z&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 146, no. 1, July 1988, p. 1-12. Research supported by the Chinese Academy

Astronomy and Astrophysics

Astrophysics

8

Eclipsing Binary Stars, Light Curve, Starspots, Mass Transfer, Quadratures, Radial Velocity, Stellar Activity, Stellar Spectrophotometry

Scientific paper

In view of the fair agreement between the photometric qptm by Zhai et al. (1984) and the spectroscopic mass ratio q5~ by Lu (1985), a simultaneous light and velocity curve solution was carried out for U Peg with the Wilson-Devinney program. For purpose of comparison, we performed separate light and velocity curve solutions and then the simultaneous photometric-spectroscopic solution. The im- proved absolute dimensions turned out to be M1 = 0.387 ± 0.004 M0, M2 = 1.167 ± 0.015 M®, R1 = 0.754 ± 0.007 R0, andR2 = 1.236 ± 0.004 R0. Based on the simultaneous solution, a thorough analysis was made for total of nine BV light curves of U Peg obtained from 1950 to 1984. It was found that (1) the complexities on light curves in 1958, 1961, and 1970 can be reproduced by spot model and there may be spot cycle with the period at least larger than 28 years; (2) the common envelope of the contact binary U Peg appears to be oscillation instability with the over-contact degree varied by a large percentage

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