Formation of close binary black holes merging due to gravitational-wave radiation


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The conditions for the formation of close-binary black-hole systems merging over the Hubble time due to gravitational-wave radiation are considered in the framework of current ideas about the evolution of massive close-binary systems. The original systems whose mergers were detected by LIGO consisted of main-sequence stars with masses of 30–100M. The preservation of the compactness of a binary black hole during the evolution of its components requires either the formation of a common envelope, probably also with a low initial abundance of metals, or the presence of a “kick”—a velocity obtained during a supernova explosion accompanied by the formation of a black hole. In principle, such a kick can explain the relatively low frequency of mergers of the components of close-binary stellar black holes, if the characteristic speed of the kick exceeds the orbital velocities of the system components during the supernova explosion. Another opportunity for the components of close-binary systems to approach each other is related to their possible motion in a dense molecular cloud.

作者简介

A. Tutukov

Institute of Astronomy, Russian Academy of Sciences

Email: cherepashchuk@gmail.com
俄罗斯联邦, ul. Pyatnitskaya 48, Moscow, 119017

A. Cherepashchuk

Sternberg Astronomical Institute

编辑信件的主要联系方式.
Email: cherepashchuk@gmail.com
俄罗斯联邦, Universitetskii pr. 13, Moscow, 119992

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