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The Formation of Subdwarf B Stars

Published online by Cambridge University Press:  12 April 2016

Zhanwen Han ,
Philipp Podsiadlowski ,
Pierre F.L. Maxted ,
Tom R. Marsh  and
Natasha Ivanova
Zhanwen Han
Affiliation:
Yunnan Observatory, NAOC, CAS, Kunming 650011, P. R., China
Philipp Podsiadlowski
Affiliation:
Astrophysics, NAPL, Oxford University, Keble Road, Oxford OX1 3RH, UK
Pierre F.L. Maxted
Affiliation:
Department of Physics, Keele University, Staffordshire ST5 5BG, UK
Tom R. Marsh
Affiliation:
University of Southampton, Department of Physics & Astronomy, Highfield, Southampton S017 1BJ, UK
Natasha Ivanova
Affiliation:
Department of Physics & Astronomy, Northwestern University, Evanston, IL 60208, USA

Abstract

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We performed full binary evolution calculations and carried out binary population synthesis studies in order to investigate the formation of subdwarf B (sdB) stars via the channels of stable Roche lobe overflow (RLOF), common envelope ejection and helium white dwarf mergers. Our model is successful in the explanation of observational properties of sdB stars, e.g. we explained the orbital period – minimum companion mass (log P – Mcomp) diagram, the effective temperature – surface gravity (Teff – log g) diagram, the orbital period distribution, the log(gθ4) (θ = 5040/Teff) distribution, the mass function distribution, the binary fraction of sdB stars, the fraction of sdB binaries with WD companions, the birth rates, the space number densities, etc. We conclude that (a) the first RLOF needs to be more stabilized than commonly assumed, (b) the first stable RLOF is not conservative, (c) common envelope ejection is very efficient.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 187: Exotic Stars as Challenges to Evolution , 2002 , pp. 285 - 290
Copyright
Copyright © Astronomical Society of the Pacific 2002

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