1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit

Warning

This publication doesn't include Faculty of Economics and Administration. It includes Faculty of Science. Official publication website can be found on muni.cz.
Authors

ZHANG B. QIAN Shengbang ZEJDA Miloslav ZHU Liying LIU Nianping

Year of publication 2017
Type Article in Periodical
Magazine / Source New Astronomy
MU Faculty or unit

Faculty of Science

Citation
Doi http://dx.doi.org/10.1016/j.newast.2017.01.007
Field Astronomy and astrophysics
Keywords Binary; Eclipsing binary; Short-period limit; Light curves
Description First CCD photometric light curves of the eclipsing binary system 1SWASP J200503.05-343726.5 are presented. Our complete light curves in V, R and I bands using the Bessell filter show an out-of-eclipsing distortion, which means that the components of the system may be active. The preliminary photometric solutions with a cool star-spot are derived by using the 2013 version of the Wilson-Devinney (W-D) code. The photometric solutions suggest that 1SWASP J200503.05-343726.5 is a shallow-contact eclipsing binary(f = 9.0%) with a mass ratio of q= 1.0705, which is very high for late-type binary systems near the period limit. The primary component is about 230 K hotter than the secondary component. Based on our new CCD eclipse times, the orbital period change was analyzed. According to 0 C diagram, the orbital period of the 1SWASP 1200503.05-343726.5 shows an increase at a rate of <(P)over dot> = +5.43 x 10(-8) days year(-1). The period increase may be caused by mass transfer from the less massive component to the more massive one. This shallow-contact system may be formed from a detached short-period binary via orbital shrinkage because of dynamical interactions with a third component or by magnetic braking. (C) 2017 Elsevier B.V. All rights reserved.
Related projects:

You are running an old browser version. We recommend updating your browser to its latest version.