First photometric study of the W UMa system GSC 1042-2191 |
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| Institution: | 1. Department of Physics, Faculty of Arts and Sciences, Çanakkale Onsekiz Mart University, Terzio?lu Kampüsü, TR-17020 Çanakkale, Turkey;2. Department of Space Sciences and Technologies, Faculty of Arts and Sciences, Çanakkale Onsekiz Mart University, Terzio?lu Kampüsü, TR-17020 Çanakkale, Turkey;3. Astrophysics Research Centre and Observatory, Çanakkale Onsekiz Mart University, Terzio?lu Kampüsü, TR-17020 Çanakkale, Turkey;1. Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital 263002, India;2. School of Studies in Physics and Astrophysics, Pt. Ravishankar Shukla University, Amanaka G.E. Road, Raipur 492010, India;3. Department of Physics and Institute of Theoretical and Computational Physics, University of Crete, GR-71003 Heraklion, Greece;4. ESL, Foundation for Research and Technology, Heraklion 71110, Greece;5. Department of Physics, The College of New Jersey, PO Box 7718, Ewing, NJ 08628-0718, USA;1. Key Laboratory of Space Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road Chaoyang District, Beijing 100012, P.R.China;2. University of Chinese Academy of Sciences, Shijingshan District, Beijing 100049, P.R.China;1. Department of Physics and Astronomy, Shumen University, Shumen 9700, Bulgaria;2. Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Mexico;1. Yunnan Observatories, Chinese Academy of Sciences (CAS), P.O. Box 110, 650011 Kunming, PR China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650011 Kunming, PR China;3. University of the Chinese Academy of Sciences, Yuquan Road 19#, Sijingshang Block, 100049 Beijing, PR China |
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| Abstract: | We present new photometric observations covering eight minima times for the eclipsing binary GSC 1042-2191. The light curves in colors were analyzed by using WD-code for the system parameters. Eight minima times were obtained from the new observations. The system is found a low mass ratio (q = 0.148), A-type over-contact binary with a fill out parameter of f = 65.01 ± 12.18%. The preliminary absolute dimensions (M1= 1.26 ± 0.06 M⊙, M2 = 0.18 ± 0.06 M⊙, R1 = 1.54 ± 0.20 R⊙, R2 = 0.69 ± 0.01 R⊙, =3.30 ± 0.30 L⊙ and = 0.59 ± 0.20 L⊙) indicate the very much oversized and over-luminous secondary component, by assuming the present luminosity of the secondary is its main sequence luminosity, we predict the original mass is about 0.8 M⊙, this means the present secondary could be transferred and/or lost 77% of its original mass and only its core is left. |
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