Formation of close binary black holes merging due to gravitational-wave radiation |
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| Authors: | A V Tutukov A M Cherepashchuk |
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| Institution: | 1.Institute of Astronomy, Russian Academy of Sciences,Moscow,Russia;2.Sternberg Astronomical Institute,Lomonosov Moscow State University,Moscow,Russia |
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| Abstract: | 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. |
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