Period and light-curve study of the contact eclipsing binary V523 Cas |
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| Institution: | 1. Department of physics, Faculty of science, University of Birjand, Iran and Dr. Mojtahedi observatory, University of Birjand, Iran;2. Department of Physics, Shahid Beheshti University, Evin, Tehran 19839, Iran;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. Instituto de Astronomía, Universidad Nacional Autónoma de México, Circuito Exterior, Ciudad Universitaria, Apartado Postal 70-543, 04510, D.F., México;2. Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA;1. Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, China;3. University of the Chinese Academy of Sciences, Beijing 100049, China;1. Via Molinetto 35, 26845 Triulza di Codogno (LO), Italy;2. Via Don G. Minzoni 26/D, 20020 Magnago (MI), Italy;3. Via Zoncada 51, 26845 Codogno (LO), Italy |
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| Abstract: | CCD photometry of the eclipsing W Uma binary system V523 Cas in U, B, V and RC filters was carried out during eight nights in 2012. The physical and geometrical parameters of this system are obtained. A possible pulsation period of one of the components is obtained by analyzing the residuals of the ephemeris light curve. Our observations contain 16 times of minimum light. We combined these with all available published times of minimum. By fitting a quadratic curve to the O-C values, a new ephemeris of the system is calculated. By attributing the period change to mass transfer, we find a mass transfer rate of . Also, Period (80.58 yr) and the minimum mass (0.3 M⊙) of a possible third body is estimated. In addition, the possible existence of a fourth body with a mass of order 0.15 M⊙ is discussed. These third and fourth bodies could be low-mass main-sequence stars (red dwarfs). |
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