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Black holes: The next generation-repeated mergers in dense star clusters and their gravitational-wave properties
Rodriguez, Carl L.1; Zevin, Michael2,3; Amaro-Seoane, Pau4,5,7,8; Chatterjee, Sourav9; Kremer, Kyle2,3; Rasio, Frederic A.2,3; Ye, Claire S.2,3
2019-08-27
Source PublicationPHYSICAL REVIEW D
ISSN2470-0010
Volume100Issue:4Pages:15
AbstractWhen two black holes merge in a dense star cluster, they form a new black hole with a well-defined mass and spin. If that "second-generation" black hole remains in the cluster, it will continue to participate in dynamical encounters, form binaries, and potentially merge again. Using a grid of 96 dynamical models of dense star clusters and a cosmological model of cluster formation, we explore the production of binary black hole mergers where at least one component of the binary was forged in a previous merger. We create four hypothetical universes where every black hole born in the collapse of a massive star has a dimensionless Kerr spin parameter, chi(birth), of 0.0, 0.1, 0.2, or 0.5. We show that if all stellar-born black holes are nonspinning (chi(birth) = 0.0), then more than 10% of merging binary black holes from clusters have components formed from previous mergers, accounting for more than 20% of the mergers from globular clusters detectable by LIGO/Virgo. Furthermore, nearly 7% of detectable mergers would have a component with a mass greater than or similar to 55 M-circle dot, placing it clearly in the mass "gap" region where black holes cannot form from isolated collapsing stars due to the pulsational-pair instability mechanism. On the other hand, if black holes are born spinning, then the contribution from these second-generation mergers decreases, making up as little as 1% of all detections from globular clusters when chi(birth) = 0.5. We make quantitative predictions for the detected masses, mass ratios, and spin properties of first- and second-generation mergers from dense star clusters, and show how these distributions are highly sensitive to the birth spins of black holes.
DOI10.1103/PhysRevD.100.043027
Language英语
Funding ProjectPappalardo Postdoctoral Fellowship at MIT ; NASA[NNX14AP92G] ; NSF at Northwestern University[AST-1716762] ; Ramon y Cajal Programme of the Ministry of Economy, Industry and Competitiveness of Spain ; COST Action GWverse[CA16104] ; Kavli Foundation ; DNRF ; NSF[PHY-1607611]
WOS Research AreaAstronomy & Astrophysics ; Physics
WOS SubjectAstronomy & Astrophysics ; Physics, Particles & Fields
WOS IDWOS:000482854800002
PublisherAMER PHYSICAL SOC
Citation statistics
Document Type期刊论文
Identifierhttp://ir.amss.ac.cn/handle/2S8OKBNM/35559
Collection中国科学院数学与系统科学研究院
Corresponding AuthorRodriguez, Carl L.
Affiliation1.MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave,37-664H, Cambridge, MA 02139 USA
2.Northwestern Univ, CIERA, 2145 Sheridan Rd, Evanston, IL 60208 USA
3.Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA
4.CSIC, Inst Space Sci ICE, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain
5.IEEC, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain
6.Kavli Inst Astron & Astrophy, Beijing 100871, Peoples R China
7.Chinese Acad Sci, Acad Math & Syst Sci, Inst Appl Math, Beijing 100190, Peoples R China
8.TU Berlin, Zentrum Astron & Astrophys, Hardenbergstr 36, D-10623 Berlin, Germany
9.Tata Inst Fundamental Res, Dept Astron & Astrophys, Homi Bhabha Rd, Mumbai, Maharashtra, India
Recommended Citation
GB/T 7714
Rodriguez, Carl L.,Zevin, Michael,Amaro-Seoane, Pau,et al. Black holes: The next generation-repeated mergers in dense star clusters and their gravitational-wave properties[J]. PHYSICAL REVIEW D,2019,100(4):15.
APA Rodriguez, Carl L..,Zevin, Michael.,Amaro-Seoane, Pau.,Chatterjee, Sourav.,Kremer, Kyle.,...&Ye, Claire S..(2019).Black holes: The next generation-repeated mergers in dense star clusters and their gravitational-wave properties.PHYSICAL REVIEW D,100(4),15.
MLA Rodriguez, Carl L.,et al."Black holes: The next generation-repeated mergers in dense star clusters and their gravitational-wave properties".PHYSICAL REVIEW D 100.4(2019):15.
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