The evolution of binary systems

doi:10.1017/CBO9781139343268.003

2 - The evolution of binary systems

Published online by Cambridge University Press: 05 January 2014

Philipp Podsiadlowski

Edited by

Ignacio González Martínez-País ,

Tariq Shahbaz and

Jorge Casares Velázquez

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Philipp Podsiadlowski: Affiliation:
University of Oxford
Ignacio González Martínez-País: Affiliation:
Instituto de Astrofísica de Canarias, Tenerife
Tariq Shahbaz: Affiliation:
Instituto de Astrofísica de Canarias, Tenerife
Jorge Casares Velázquez: Affiliation:
Instituto de Astrofísica de Canarias, Tenerife

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Summary

Abstract

One of the most important environments in which accretion disks are found occur in interacting binaries. In this chapter I review the main properties of binary systems and the most important types of binary interactions, stable and unstable mass transfer, the role of mass loss, mass accretion, and, in the most dramatic case, the merging of the two binary components. I particularly emphasize the evolutionary context in which these interactions occur and illustrate this using numerous examples of different types of binaries of current research interest. These include hot subdwarfs; symbiotic binaries; binary supernova progenitors, including the progenitors of type Ia supernovae and potential progenitors of long-duration gamma-ray bursts; low-, intermediate-, and high-mass X-ray binaries, containing both neutron stars and black holes; and their descendants, including binary millisecond pulsars, Thorne-Żytkow objects, and short-duration gamma-ray bursts.

2.1 Introduction

One of the main sites for accretion disks are interacting binary systems. Indeed, the majority of stars are found in binary systems, and in many cases (up to ~50%), they are close enough that mass flows from one star to the other, in many cases forming an accretion disk. This can happen for a wide variety of different systems: systems containing two normal nondegenerate stars, or one compact star (white dwarf [WD], neutron star [NS], or black hole [BH]), or even two compact stars of various combinations.

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Type: Chapter
Information: Accretion Processes in Astrophysics , pp. 45 - 88

DOI: https://doi.org/10.1017/CBO9781139343268.003 [Opens in a new window]

Publisher: Cambridge University Press

Print publication year: 2014

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