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The Formation of Compact Objects in Binary Systems

Published online by Cambridge University Press:  14 August 2015

E.P.J. van den Heuvel
E.P.J. van den Heuvel*
Affiliation:
Astronomical Institute, University of Amsterdam, the Netherlands Astrophysical Institute, Vrije Universiteit, Brussels, Belgium

Abstract

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The various ways in which compact objects (neutron stars and black holes) can be formed in interacting binary systems are qualitatively outlined on the basis of the three major modes of binary interaction identified by Webbink (1980). Massive interacting binary systems (M1 ≳ 10–12 M⊙) are, after the first phase of mass transfer expected to leave as remnants:

(i) compact stars in massive binary systems (mass ≳ 10 M⊙) with a wide range of orbital periods, as remnants of quasi-conservative mass transfer; these systems later evolve into massive X-ray binaries.

(ii) short-period compact star binaries (P ~ 1–2 days) in which the companion may be more massive or less massive than the compact object; these systems have high runaway velocities (≳ 100 km/sec) and start out with highly eccentric orbits, which are rapidly circularized by tidal forces; they may later evolve into low-mass X-ray binaries;

(iii) single runaway compact objects with space velocities of ~ 102 to 4.102 km/sec; these are expected to be the most numerous compact remnants.

Compact star binaries may also form from Cataclysmic binaries or wide binaries in which an O-Ne-Mg white dwarf is driven over the Chandrasekhar limit by accretion.

Type
Session 4: Mass Exchange on Close Binary Stars and the Effect on Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 93: Fundamental Problems in the Theory of Stellar Evolution , 1981 , pp. 155 - 175
Copyright
Copyright © Reidel 1981 

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