The Mass of the sdB Primary of the Binary HS 2333+3927
Heber, U.; Drechsel, H.; Karl, C.; Ostensen, R.; Folkes, S.; Napiwotzki, R.; Altmann, M.; Cordes, O.; Solheim, J.E.; Voss, B.; Koester, D.
Citation: Heber , U , Drechsel , H , Karl , C , Ostensen , R , Folkes , S , Napiwotzki , R , Altmann , M , Cordes , O , Solheim , J E , Voss , B & Koester , D 2005 , ' The Mass of the sdB Primary of the Binary HS 2333+3927 ' . in In: Procs of the 14th European Workshop on White Dwarfs - ASP Conference Papers 334 . Astronomical Society of the Pacific , pp. 357-362 .
Short period sdB binaries with cool companions are crucial to understand pre-CV evolution, because they will evolve into cataclysmic variables, when the sdB will have left the extended horizontal branch. Recently we discovered the sixth such system, HS 2333+3927, consisting of an sdB star and an M dwarf (period: 0.172 d) with a very strong re°ection e®ect, but no eclipses. The re°ection is stronger than in any of the other similar systems which renders a quantitative spectral analysis very di±cult because the Balmer line pro¯les may be disturbed by the re°ected light. A spectroscopic analysis results in Te® = 36 500 K, log g = 5.70, and log(nHe=nH) = ¡2:15. Mass-radius relations were derived from the results of the analysis of light and radial-velocity curves. Comparison with the mass-radius relation derived from the surface gravity of the sdB star favours a rather low mass of 0.38 M¯ for the primary. The mass of the companion is 0.29 M¯. HS 2333+3927 is the only known sdB+dM system with a period above the CV period gap.
Original paper can be found at: http://www.astrosociety.org/pubs/cs/328.html--Copyright Astronomical Society of the Pacific
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