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  The Formation and Gravitational-Wave Detection of Massive Stellar Black-Hole Binaries

Belczynski, K., Buonanno, A., Cantiello, M., Fryer, C. L., Holz, D. E., Mandel, I., et al. (2014). The Formation and Gravitational-Wave Detection of Massive Stellar Black-Hole Binaries. Astrophysical Journal, 789(2): 120. doi:10.1088/0004-637X/789/2/120.

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Datensatz-Permalink: http://hdl.handle.net/11858/00-001M-0000-0023-F9BC-4 Versions-Permalink: http://hdl.handle.net/11858/00-001M-0000-0024-25BF-2
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1403.0677.pdf (Preprint), 440KB
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0004-637X_789_2_120.pdf (beliebiger Volltext), 580KB
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 Urheber:
Belczynski, Krzysztof, Autor
Buonanno, A.1, 2, Autor              
Cantiello, Matteo, Autor
Fryer, Chris L., Autor
Holz, Daniel E., Autor
Mandel, Ilya, Autor
Miller, M. Coleman, Autor
Walczak, Marek, Autor
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:1933290              
2Maryland Center for Fundamental Physics & Joint Space-Science Institute, Department of Physics, University of Maryland, escidoc:persistent22              

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Schlagwörter: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Zusammenfassung: If binaries consisting of two 100 Msun black holes exist they would serve as extraordinarily powerful gravitational-wave sources, detectable to redshifts of z=2 with the advanced LIGO/Virgo ground-based detectors. Large uncertainties about the evolution of massive stars preclude definitive rate predictions for mergers of these massive black holes. We show that rates as high as hundreds of detections per year, or as low as no detections whatsoever, are both possible. It was thought that the only way to produce these massive binaries was via dynamical interactions in dense stellar systems. This view has been challenged by the recent discovery of several stars with mass above 150 Msun in the R136 region of the Large Magellanic Cloud. Current models predict that when stars of this mass leave the main sequence, their expansion is insufficient to allow common envelope evolution to efficiently reduce the orbital separation. The resulting black-hole--black-hole binary remains too wide to be able to coalesce within a Hubble time. If this assessment is correct, isolated very massive binaries do not evolve to be gravitational-wave sources. However, other formation channels exist. For example, the high multiplicity of massive stars, and their common formation in relatively dense stellar associations, opens up dynamical channels for massive black hole mergers (e.g., via Kozai cycles or repeated binary-single interactions). We identify key physical factors that shape the population of very massive black-hole--black-hole binaries. Advanced gravitational-wave detectors will provide important constraints on the formation and evolution of very massive stars.

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 Datum: 2014-03-032014-05-272014
 Publikationsstatus: Im Druck publiziert
 Seiten: ApJ accepted, extended description of modeling
 Ort, Verlag, Ausgabe: -
 Inhaltsverzeichnis: -
 Art der Begutachtung: -
 Identifikatoren: arXiv: 1403.0677
URI: http://arxiv.org/abs/1403.0677
DOI: 10.1088/0004-637X/789/2/120
 Art des Abschluß: -

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Titel: Astrophysical Journal
Genre der Quelle: Zeitschrift
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Ort, Verlag, Ausgabe: Chicago, IL : University of Chicago Press for the American Astronomical Society
Seiten: - Band / Heft: 789 (2) Artikelnummer: 120 Start- / Endseite: - Identifikator: ISSN: 0004-637X
CoNE: http://pubman.mpdl.mpg.de/cone/journals/resource/954922828215_2