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Stellar Evolution and the Formation of Neutron Stars in Binary Systems

  • Chapter
High Energy Phenomena Around Collapsed Stars

Part of the book series: NATO ASI Series ((ASIC,volume 195))

Abstract

The evolution of single stars is reviewed and the possible types of remnants are discussed.

Subsequently, mechanisms for the formation of neutron stars in binary systems are reviewed. In close binary systems, stars in the (zero-age) mass range ~ 10 to > 40 MO are expected to leave neutron stars as remnants. In wide binaries and for single stars the lower limit is reduced to about ~ 8 MO. The precise value of the lower limit depends on various input parameters, especially on the treatment of convection.

Accretion-induced collapse (AIC) of a white dwarf of suitable mass and chemical composition is a second viable mechanism for the formation of neutron stars in binary systems. Evidence is summarized indicating that both in the wide radio pulsar binaries and in the bright galactic bulge X-ray sources that exhibit Quasi Periodic Oscillations (QPO) the neutron stars were formed by AIC.

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Authors and Affiliations

  1. Astronomical Institute, University of Amsterdam, The Netherlands

    E. P. J. van den Heuvel

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  1. E. P. J. van den Heuvel
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  1. Arcetri Astrophysical Observatory, Florence, Italy

    F. Pacini

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van den Heuvel, E.P.J. (1987). Stellar Evolution and the Formation of Neutron Stars in Binary Systems. In: Pacini, F. (eds) High Energy Phenomena Around Collapsed Stars. NATO ASI Series, vol 195. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3823-6_1

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  • DOI: https://doi.org/10.1007/978-94-009-3823-6_1

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