Photometric Investigation of the Contact Binary GU Ori with High Metallicity

作     者：Zhou, X. Qian, S.-B. Soonthornthum, B. Poshyachinda, S. Zhu, L.-Y. Liu, N.-P. Sarotsakulchai, T. Fang, X.-H. 

作者机构： P.O. Box 110 Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang Dis-trict Beijing100012 China University of the Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China National Astronomical Research Institute of Thailand 260 Moo 4 T. Donkaew A. MaerimChiangmai50180 Thailand 

出 版 物：《arXiv》 (arXiv)

年 卷 期：2018年

核心收录：

主　　题：Photometry 

摘      要：GU Ori was observed with the 1m telescope at Yunnan Observatories in 2005. To determine its physical properties, the Wilson-Devinney program is used. The results reveal that GU Ori is a W-subtype shallow contact binary with a more massive but cooler star 2. The mass of its two component stars are estimated to be M1 = 0.45M☉, M2 = 1.05M☉. The O’Connell effect was reported to be negative on the light curves observed in 2005. However, it changed to a positive one on the light curves observed from 2011 to 2012. The mean surface temperatures of star 2 (T2) determined by the two sets of light curves were different, which may result from stellar activities. The O - C diagram shows that the period of GU Ori is decreasing at a rate of dP/dt = −6.24 × 10−8day · year−1, which may be caused by mass transfer from star 2 to star 1 with a rate of dMdt2 = −2.98 × 10−8M☉/year. GU Ori is a contact binary with quite high metallicity. Copyright © 2018, The Authors. All rights reserved.