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Mass Loss and Evolution of O-Type Stars pp 401–407Cite as

Evolution of Massive Common Envelope Binaries and Mass Loss

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Part of the book series: International Astronomical Union/Union Astronomique Internationale ((IAUS,volume 83))

Abstract

A way of treatment of evolution of common envelope binaries based only on the laws of conservation of energy and angular momentum is suggested. It is shown that the final configuration depends on masses of components and initial period of the system, and on parameters describing friction in the envelope, and mass loss by the system. Possible final stages for massive binaries are either a Thorne-Zytkow type object for initially close binaries or a Wolf-Rayet star in pair with a relativistic compact remnant for wider ones. In the course of disruption of the latter system with orbital periods up to several hours very high space velocity (up to 500 km/s) pulsars can arise.

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References

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Author information

Authors and Affiliations

  1. Astronomical Council of the USSR Academy of Sciences, Soviet Union

    A. Tutukov & L. Yungelson

Authors
  1. A. Tutukov
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  2. L. Yungelson
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Editor information

Editors and Affiliations

  1. Joint Institute for Laboratory Astrophysics, University of Colorado, Boulder, USA

    P. S. Conti

  2. Astrophysical Institute, Vrije Universiteit, Brussels, Belgium

    C. W. H. De Loore

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© 1979 International Astronomical Union

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Tutukov, A., Yungelson, L. (1979). Evolution of Massive Common Envelope Binaries and Mass Loss. In: Conti, P.S., De Loore, C.W.H. (eds) Mass Loss and Evolution of O-Type Stars. International Astronomical Union/Union Astronomique Internationale, vol 83. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-9452-2_56

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  • DOI: https://doi.org/10.1007/978-94-009-9452-2_56

  • Publisher Name: Springer, Dordrecht

  • Print ISBN: 978-90-277-0989-9

  • Online ISBN: 978-94-009-9452-2

  • eBook Packages: Springer Book Archive

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