Abstract
Hot subdwarf B (sdB), O (sdO) and sdOB stars (see Greenstein&Sargent (1974) for pioneered work in this field) are subluminous evolved stars, on their way to becoming white dwarfs. They have long been known as stars burning helium in their cores, covered by a very thin hydrogen layer with negligible luminosity. In the log(g)-Teff plane, sdB and sdOB stars are narrowly distributed along the so-called ’Extended Horizontal Branch’.
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© 1997 Kluwer Academic Publishers
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Ulla, A., Thejll, P. (1997). Hot Subdwarfs in Binaries: Evolution and Physical Parameters. In: Docobo, J.A., Elipe, A., McAlister, H. (eds) Visual Double Stars: Formation, Dynamics and Evolutionary Tracks. Astrophysics and Space Science Library, vol 223. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-1477-3_27
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DOI: https://doi.org/10.1007/978-94-009-1477-3_27
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