1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit
| Authors | |
|---|---|
| Year of publication | 2017 |
| Type | Article in Periodical |
| Magazine / Source | New Astronomy |
| MU Faculty or unit | |
| 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: |