The close binary BS Vulpeculae |
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| Affiliation: | 1. Mountain Ash Observatory, 1393 Garvin Street, Prince George, BC, V2M 3Z1, Canada;2. Desert Blooms Observatory, Benson, AZ, United States;3. Canadian Astronomy Data Centre, which is operated by the Dominion Astrophysical Observatory for the National Research Council of Canada''s Herzberg Institute of Astrophysics, Canada;1. Yunnan Observatories, Chinese Academy of Sciences (CAS), P.O. Box 110, Kunming 650216, China;2. National Astronomical Research Institute of Thailand, Ministry of Higher Education Science Research and Innovation, 260 Moo 4, T. Donkaew, A. Maerim, Chiangmai, 50180, Thailand;3. Guizhou Provincial Key Laboratory of Radio Data Processing, School of Physics and Electronic Sciences, Guizhou Education University, Guiyang 550001, China;4. Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, P.O. Box 110, Kunming 650216, China;5. Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, P.R. China;6. University of Chinese Academy of Sciences, Yuquan Road 19#, Sijingshang Block, Beijing 100049, China;1. Department of Mathematics, SSJ Campus, Kumaun University, Almora 263601, India;2. Department of Mathematics, National Defence Academy, Khadakwasla, Pune 411023, India;3. Graphic Era Hill University, Bhimtal Campus, Sattal Road, Bhimtal 263132, India;1. The International Occultation Timing Association Middle East section, Iran;2. Adana Organised Industrial Zones Vocational School of Technical Science, University of Çukurova, 01410, Adana, Turkey;3. Space Science and Solar Energy Research and Application Center (UZAYMER), University of Çukurova, 01330, Adana, Turkey;1. Department of Physics and Astronomy, Shumen University, Shumen 9700, Bulgaria;2. Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Mexico;3. Department of Astronomy, Beijing Normal University, Beijing 100875, China;1. Astronomical Institute, Faculty of Mathematics and Physics, Charles University Prague, CZ-180 00 Praha 8, V Holešovičkách 2, Czech Republic;2. Variable Star and Exoplanet Section, Czech Astronomical Society, Czech Republic;3. Institute of Physics, Czech Academy of Sciences, Na Slovance 1999/2, Praha 8 CZ-182 21, Czech Republic;4. Astronomical Institute, Academy of Sciences, Fričova 298, Ondřejov CZ-251 65, Czech Republic;5. Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava, Bezručovo nám. 13, Opava CZ-746 01, Czech Republic;1. Mountain Ash Observatory, 1393 Garvin Street, Prince George, BC, V2M 3Z1, Canada;2. Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, College of New Caledonia, Prince George, B.C., Canada |
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| Abstract: | The first radial velocity curves for BS Vul have been obtained. Combined with new light curve data, simultaneous Roche-based light curve analyses have been carried out using the 2003 version of the Wilson-Devinney code. New values for the masses, radii, and luminosities have been obtained: M1 = 2.03 (8) M ʘ, M 2 = 0.68 (3) M ʘ, R1 = 1.71 (2) Rʘ, R2 = 1.03 (2) Rʘ, L1 = 5.4 (5) L ʘ, and L 2 = 0.41 (4) L ʘ. Comparison with re-modelled data from De Bernardi and Skaltriti (1979) revealed good agreement although temperature T2 there seemed to be significantly lower. There was also reasonable agreement with the results from the photometric analysis of Zhu et al. (2012). Reference to the sample of close binary stars from Yakut and Eggleton (2005) and the ZAMS suggests that both stars are evolved. |
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