An updated period analysis for ER Orionis: A definitive solution |
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| Institution: | 1. Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, China;3. University of Chinese Academy of Sciences, Beijing 100049, China;1. Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, TR-06100 Tandoğan, Ankara, Turkey;2. Department of Astronomy and Satellite Geodesy, Kazan Federal University (KFU), 420008 Kazan, Russia;3. Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8550, Japan;4. Academy of Sciences of Tatarstan, Bauman Str, 20, 420111 Kazan, Russia;5. Ege University, Faculty of Science, Department of Astronomy and Space Sciences, TR-35100 Bornova, İzmir, Turkey;6. Okayama Astrophysical Observatory, National Astronomical Observatory, Honjo 3037-5, Kamogata, Okayama 719-0232, Japan;7. Advanced Technology Center, National Astronomical Observatory, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan |
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| Abstract: | An updated period analysis for the overcontact eclipsing binary ER Orionis is presented. Featured is an improved derivation of parameters for the light time effect (LTE) due to the third star (in actuality, a pair of stars) utilising the latest set of eclipse timings. The very good fit between the eclipse timing differences (ETD) plot (otherwise known as an O–C diagram) and the theoretical ETD curve makes possible an improved determination of the rate of mass interchange between the binary pair, dm1/dt = +1.83(6) × 10−7 Mʘ/year. In addition, the mass of the companion system (in actuality, m3 sin i) and the elements of its orbit were computed. A suggestion is made for a method of future determination of the inclination of the orbit of the companion system. |
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| Keywords: | Stars: binaries: eclipsing Stars: fundamental parameters Stars: individual (ER Ori) |
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