Orbital variations and outbursts of the unusual variable star V1129 Centauri |
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| Institution: | 1. Department of Physics, & Centre for Theoretical Studies, IIT Kharagpur, Pin: 721302, India;2. National Centre For Radio Astrophysics, Post Bag 3, Ganeshkhind, Pune 411007, India;3. Department of Physics, Indian Institute of Science, Bangalore 560012, India;4. Department of Physics and Meteorology & Centre for Theoretical Studies, IIT Kharagpur, 721302 India;5. Department of Physics, Jadavpur University, Kolkata 700032, India;6. Dept of Physics and Astronomy, University of the Western Cape, Robert Sobukwe Road, Bellville 7535, South Africa;7. SKA SA, The Park, Park Road, Pinelands 7405, South Africa;8. Department of Physics, IIT (BHU), Varanasi 221005, India;1. Department of Physics, V V College of Engineering, Tirunelveli, 627 657 India;2. Department of Physics, VVV College for Women, Virudhunagar, 626 001 India;3. Research and Development Centre, Bharathiar University, Coimbatore, 641 046 India;4. Physics Research Centre, VHNSN College, Virudhunagar, 626 001 India;1. Department of Mathematics, Gauhati University, Guwahati-14, India;2. Department of Mathematics, A.D.P. College, Nagaon-02, India;1. Department of Astronomy, Nanjing University, Nanjing, Jiangshu 210000, China;2. College of Electronic and Communication Engineering, Hainan Tropical Ocean University, Sanya 572022, China;3. Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China;1. Astronomical Institute, Charles University in Prague, Faculty of Mathematics and Physics, V Hole?ovi?kách 2, CZ-18000 Prague 8, Czech Republic;2. Astronomical Institute (v. v. i.), Czech Academy of Sciences, Fri?ova 298, CZ-25165 Ond?ejov, Czech Republic |
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| Abstract: | The variable star V1129 Cen is classified in the GCVS as being of β Lyr type. Unusual for such stars, it exhibits outbursts roughly once a year, lasting for ～ 40 days. For this reason, a relationship to the dwarf novae has been suspected. Here, for the first time a detailed analysis of the light curve of the system is presented. Based on observations with high time resolution obtained at the Observatório do Pico dos Dias and on the long term ASAS light curve the orbital variations of the system are studied. They are dominated by ellipsoidal variations and partial eclipses of a probably slightly evolved F2 star in a binary with an orbital period of 21h 26m. Comparison with the characteristics of dwarf novae show that the observational properties of V1129 Cen can be explained if it is just another dwarf novae, albeit with an unusually bright and early type mass donor which outshines the accretion disk and the mass gainer to a degree that many normal photometric and spectroscopic hallmarks of cataclysmic variables remain undetected. |
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