First analysis of eight Algol-type binaries: EI Aur,XY Dra,BP Dra,DD Her,VX Lac,WX Lib,RZ Lyn,and TY Tri |
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| Institution: | 1. High Energy Physics Division, Argonne National Laboratory, Lemont, IL 60439, USA;2. Mathematics and Computer Science Division, Argonne National Laboratory, Lemont, IL 60439, USA;3. Kavli Institute for Cosmological Physics, The University of Chicago, 5640 S. Ellis Ave., Chicago, IL 60637, USA;4. Computation Institute, The University of Chicago, Chicago, IL 60637, USA;5. Argonne Leadership Computing Facility, Argonne National Laboratory, Lemont IL 60439, USA;6. Department of Physics, University of Chicago, Chicago, IL 60637, USA;7. Computer, Computational, and Statistical Sciences Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA;8. Kitware, 28 Corporate Drive, Clifton Park, NY 12065, USA;9. Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 90095, USA;10. Department of Electrical Engineering and Computer Science, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA;1. Department of Physics and Astronomy, Sejong University, Gwangjin-gu, Seoul 143-747, Republic of Korea;2. Istituto Nazionale di Astrofisica Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, Napoli 80131, Italy;3. International Center for Relativistic Astrophysics, Piazzale della Repubblica 2, Pescara 65122, Italy;1. Department of Astronomy, Beijing Normal University, Beijing 100875, China;2. Xingjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China;3. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China;1. Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China;2. Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China;3. University of Chinese Academy of Sciences, No. 19A Yuquan Road, Beijing 100049, China |
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| Abstract: | The available photometry from the online databases were used for the first light curve analysis of eight eclipsing binary systems EI Aur, XY Dra, BP Dra, DD Her, VX Lac, WX Lib, RZ Lyn, and TY Tri. All these stars are of Algol-type, having the detached components and the orbital periods from 0.92 to 6.8 days. For the systems EI Aur and BP Dra the large amount of the third light was detected during the light curve solution. Moreover, 468 new times of minima for these binaries were derived, trying to identify the period variations. For the systems XY Dra and VX Lac the third bodies were detected with the periods 17.7, and 49.3 years, respectively. |
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