2017/12/26 by Bin Zhang, Sheng-Bang Qian, Sheng-bang Qian +6
Physics and Astronomy · #Angular momentum #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Binary number #Contact binary #Diagram #Light curve #Mass ratio #Orbital period #Shrinkage #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1088/1674-4527/18/3/30
arxiv created 2017/12/26 · openalex created_date 2018/01/05 · openalex publication_date 2018/03/01 · arxiv updated 2018/04/04 · openalex updated_date 2026/08/06
Abstract In this paper, CCD photometric light curves for the short-period eclipsing binary 1SWASP J140533.33+114639.1 (hereafter J1405) in the BV R bands are presented and analyzed using the 2013 version of the Wilson-Devinney (W-D) code. It is discovered that J1405 is a W-subtype shallow contact binary with a contact degree of f = 7.9 ± 0.5% and a mass ratio of q = 1.55 ± 0.02. In order to explain the asymmetric light curves of the system, a cool starspot on the more massive component is employed. This shallow contact eclipsing binary may have been formed from a short-period detached system through orbital shrinkage due to angular momentum loss. Based on the ( O – C ) method, the variation of orbital period is studied using all the available times of minimum light. The ( O – C ) diagram reveals that the period is increasing continuously at a rate of dP / dt = +2.09 × 10 −7 , d yr −1 , which can be explained by mass transfer from the less massive component to the more massive one.