期刊
ASTROPHYSICAL JOURNAL
卷 854, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4357/aaa7f4
关键词
black hole physics; gravitational waves; stars: kinematics and dynamics
资金
- MEXT KAKENHI [17H06357, 17H06358, 17H06359, 15H05888, 15H02087, 15K21733]
- JSPS [15K17632, 15K17659, 26287044]
- European Research Council (ERC) under the European Union's Horizon research and innovation programme [638435]
- Hungarian National Research, Development, and Innovation Office grant [NKFIH KH-125675]
- National Science Foundation [PHY-1607761]
- Grants-in-Aid for Scientific Research [17H06077, 17H06358, 17H06357, 15K17632, 15H02087, 26287044, 15K17659, 15H05888] Funding Source: KAKEN
It has been proposed that primordial black holes (PBHs) form binaries in the radiation dominated era. Once formed, some fraction of them may merge within the age of the universe by gravitational radiation reaction. We investigate the merger rate of the PBH binaries when the PBHs have a distribution of masses around O(10) M-circle dot, which is a generalization of the previous studies where the PBHs are assumed to have the same mass. After deriving a formula for the merger time probability distribution in the PBH mass plane, we evaluate it under two different approximations. We identify a quantity constructed from the mass distribution of the merger rate density per unit cosmic time and comoving volume R (m(1), m(2)), alpha = -(m(1)+ m(2))(2)partial derivative(2) In R/partial derivative m(1)partial derivative m(2),which universally satisfies 0.97 less than or similar to alpha less than or similar to 1.05 for all binary masses independently of the PBH mass function. This result suggests that the measurement of this quantity is useful for testing the PBH scenario.
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