Kottamia 74-inch telescope discovery of the new eclipsing binary KAO-EGYPT J225702.44+523222.1.: First CCD photometry and light curve analysis |
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| Institution: | 1. Astronomy Department, National Research Institute of Astronomy and Geophysics, (NRIAG), Helwan, Cairo, Egypt;2. Kottamia Center of Scientific Excellence in Astronomy and Space Sciences (KCScE), STDF, ASRT, Cairo, Egypt;1. Observatorio Astronómico de Córdoba, Laprida 854, Córdoba, Argentina;2. CONICET, Consejo Nacional de Investigaciones Científicas y Técnicas, Argentina;1. Girijananda Chowdhury Institute of Management and Technology, Guwahati, India;2. Bhabha Atomic Research Centre, Mumbai, India;3. IUCAA, Pune, India;4. Department of Physics, Gauhati University, Guwahati, India;1. Science Faculty, Department of Astronomy and Space Sciences, Ankara University, Tando?an 06100, Ankara, Turkey;2. Graduate School of Science and Engineering, Istanbul University, Bozdo?an Kemeri Cad. 8, Vezneciler, ?stanbul, Turkey;3. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 66, Cambridge, MA 02138, USA;1. Yunnan Observatories, Chinese Academy of Sciences (CAS), P.O. Box 110, 650216 Kunming, P.R. China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650216 Kunming, P.R. China;3. University of the Chinese Academy of Sciences, Yuquan Road 19#, Sijingshang Block, 100049 Beijing, P.R. China;1. Department of Physics, Faculty of Arts and Sciences, Çanakkale Onsekiz Mart University, Terzio?lu Kampüsü, TR-17020 Çanakkale, Turkey;2. Astrophysics Research Centre and Observatory, Çanakkale Onsekiz Mart University, Terziog?lu Kampüsü, TR-17020 Çanakkale, Turkey;3. ?zmir Turk College Planetarium, 8019/21 sok. No:22, ?zmir, Turkey |
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| Abstract: | We present the first multicolor CCD photometry for the newly discovered binary system KAO-EGYPT J225702.44+523222.1. New times of light minimum and new ephemeris were obtained. The VR I light curves were analyzed using WD code, the difference in maximum light at phase 0.25 is modeled with a cool spot on the secondary component. The solution show that the system is A-subtype, overcontact binary with fill-out factor = 42% and low mass ratio, q = 0.275. The two components of spectral types K0 and K1 and the primary component is the massive one. The position of both components on the M-L and M–R relations revealed that the primary component is a main sequence star while the secondary is an evolved component. |
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