Formation of close binary black holes merging due to gravitational-wave radiation
- Авторлар: Tutukov A.V.1, Cherepashchuk A.M.2
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Мекемелер:
- Institute of Astronomy, Russian Academy of Sciences
- Sternberg Astronomical Institute
- Шығарылым: Том 61, № 10 (2017)
- Беттер: 833-847
- Бөлім: Article
- URL: https://journals.rcsi.science/1063-7729/article/view/191080
- DOI: https://doi.org/10.1134/S1063772917100092
- ID: 191080
Дәйексөз келтіру
Аннотация
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.
Авторлар туралы
A. Tutukov
Institute of Astronomy, Russian Academy of Sciences
Email: cherepashchuk@gmail.com
Ресей, ul. Pyatnitskaya 48, Moscow, 119017
A. Cherepashchuk
Sternberg Astronomical Institute
Хат алмасуға жауапты Автор.
Email: cherepashchuk@gmail.com
Ресей, Universitetskii pr. 13, Moscow, 119992
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