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Post-Newtonian dynamics in dense star clusters: Formation, masses, and merger rates of highly-eccentric black hole binaries

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Standard

Post-Newtonian dynamics in dense star clusters : Formation, masses, and merger rates of highly-eccentric black hole binaries. / Rodriguez, Carl L.; Amaro-Seoane, Pau; Chatterjee, Sourav; Kremer, Kyle; Rasio, Frederic A.; Samsing, Johan; Ye, Claire S.; Zevin, Michael.

I: Physical Review D, Bind 98, Nr. 12, 123005, 15.12.2018.

Publikation: Bidrag til tidsskriftTidsskriftartikelForskningfagfællebedømt

Harvard

Rodriguez, CL, Amaro-Seoane, P, Chatterjee, S, Kremer, K, Rasio, FA, Samsing, J, Ye, CS & Zevin, M 2018, 'Post-Newtonian dynamics in dense star clusters: Formation, masses, and merger rates of highly-eccentric black hole binaries', Physical Review D, bind 98, nr. 12, 123005. https://doi.org/10.1103/PhysRevD.98.123005

APA

Rodriguez, C. L., Amaro-Seoane, P., Chatterjee, S., Kremer, K., Rasio, F. A., Samsing, J., ... Zevin, M. (2018). Post-Newtonian dynamics in dense star clusters: Formation, masses, and merger rates of highly-eccentric black hole binaries. Physical Review D, 98(12), [123005]. https://doi.org/10.1103/PhysRevD.98.123005

Vancouver

Rodriguez CL, Amaro-Seoane P, Chatterjee S, Kremer K, Rasio FA, Samsing J o.a. Post-Newtonian dynamics in dense star clusters: Formation, masses, and merger rates of highly-eccentric black hole binaries. Physical Review D. 2018 dec 15;98(12). 123005. https://doi.org/10.1103/PhysRevD.98.123005

Author

Rodriguez, Carl L. ; Amaro-Seoane, Pau ; Chatterjee, Sourav ; Kremer, Kyle ; Rasio, Frederic A. ; Samsing, Johan ; Ye, Claire S. ; Zevin, Michael. / Post-Newtonian dynamics in dense star clusters : Formation, masses, and merger rates of highly-eccentric black hole binaries. I: Physical Review D. 2018 ; Bind 98, Nr. 12.

Bibtex

@article{5c2cfb95554e4eaea29d012951611c03,
title = "Post-Newtonian dynamics in dense star clusters: Formation, masses, and merger rates of highly-eccentric black hole binaries",
abstract = "Using state-of-the-art dynamical simulations of globular clusters, including radiation reaction during black hole encounters and a cosmological model of star cluster formation, we create a realistic population of dynamically formed binary black hole mergers across cosmic space and time. We show that in the local universe, 10{\%} of these binaries form as the result of gravitational-wave emission between unbound black holes during chaotic resonant encounters, with roughly half of those events having eccentricities detectable by current ground-based gravitational-wave detectors. The mergers that occur inside clusters typically have lower masses than binaries that were ejected from the cluster many Gyrs ago. Gravitational-wave captures from globular clusters contribute 1-2 Gpc-3 yr-1 to the binary merger rate in the local universe, increasing to 10 Gpc-3 yr-1 at z∼3. Finally, we discuss some of the technical difficulties associated with post-Newtonian scattering encounters, and how care must be taken when measuring the binary parameters during a dynamical capture.",
author = "Rodriguez, {Carl L.} and Pau Amaro-Seoane and Sourav Chatterjee and Kyle Kremer and Rasio, {Frederic A.} and Johan Samsing and Ye, {Claire S.} and Michael Zevin",
year = "2018",
month = "12",
day = "15",
doi = "10.1103/PhysRevD.98.123005",
language = "English",
volume = "98",
journal = "Physical Review D",
issn = "2470-0010",
publisher = "American Physical Society",
number = "12",

}

RIS

TY - JOUR

T1 - Post-Newtonian dynamics in dense star clusters

T2 - Formation, masses, and merger rates of highly-eccentric black hole binaries

AU - Rodriguez, Carl L.

AU - Amaro-Seoane, Pau

AU - Chatterjee, Sourav

AU - Kremer, Kyle

AU - Rasio, Frederic A.

AU - Samsing, Johan

AU - Ye, Claire S.

AU - Zevin, Michael

PY - 2018/12/15

Y1 - 2018/12/15

N2 - Using state-of-the-art dynamical simulations of globular clusters, including radiation reaction during black hole encounters and a cosmological model of star cluster formation, we create a realistic population of dynamically formed binary black hole mergers across cosmic space and time. We show that in the local universe, 10% of these binaries form as the result of gravitational-wave emission between unbound black holes during chaotic resonant encounters, with roughly half of those events having eccentricities detectable by current ground-based gravitational-wave detectors. The mergers that occur inside clusters typically have lower masses than binaries that were ejected from the cluster many Gyrs ago. Gravitational-wave captures from globular clusters contribute 1-2 Gpc-3 yr-1 to the binary merger rate in the local universe, increasing to 10 Gpc-3 yr-1 at z∼3. Finally, we discuss some of the technical difficulties associated with post-Newtonian scattering encounters, and how care must be taken when measuring the binary parameters during a dynamical capture.

AB - Using state-of-the-art dynamical simulations of globular clusters, including radiation reaction during black hole encounters and a cosmological model of star cluster formation, we create a realistic population of dynamically formed binary black hole mergers across cosmic space and time. We show that in the local universe, 10% of these binaries form as the result of gravitational-wave emission between unbound black holes during chaotic resonant encounters, with roughly half of those events having eccentricities detectable by current ground-based gravitational-wave detectors. The mergers that occur inside clusters typically have lower masses than binaries that were ejected from the cluster many Gyrs ago. Gravitational-wave captures from globular clusters contribute 1-2 Gpc-3 yr-1 to the binary merger rate in the local universe, increasing to 10 Gpc-3 yr-1 at z∼3. Finally, we discuss some of the technical difficulties associated with post-Newtonian scattering encounters, and how care must be taken when measuring the binary parameters during a dynamical capture.

UR - http://www.scopus.com/inward/record.url?scp=85059368850&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.98.123005

DO - 10.1103/PhysRevD.98.123005

M3 - Journal article

AN - SCOPUS:85059368850

VL - 98

JO - Physical Review D

JF - Physical Review D

SN - 2470-0010

IS - 12

M1 - 123005

ER -

ID: 236271302