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Nielsen, A. (2016)
Publisher: Institute of Physics Publishing
Types: Article
Subjects: Stellar-mass black holes, Physik, Astrophysics - High Energy Astrophysical Phenomena, Stars, Gravitational wave detectors, Advanced detector, X-ray techniques, Gravitation, Gravitational effects, Black holes, Gravitationswelle, Naturwissenschaften, Gravity waves
ddc: ddc:530, ddc:500

Classified by OpenAIRE into

arxiv: General Relativity and Quantum Cosmology, Astrophysics::High Energy Astrophysical Phenomena, Condensed Matter::Strongly Correlated Electrons
Black hole spin will have a large impact on searches for gravitational waves with advanced detectors. While only a few stellar mass black hole spins have been measured using X- ray techniques, gravitational wave detectors have the capacity to greatly increase the statistics of black hole spin measurements. We show what we might learn from these measurements and how the black hole spin values are influenced by their formation channels.
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    • [1] E. Abdikamalov, S. Gossan, A. M. DeMaio and C. D. Ott, arXiv:1311.3678 [astro-ph.SR].
    • [2] T. Dal Canton et al., Phys. Rev. D 90 (2014) 8, 082004 [arXiv:1405.6731 [gr-qc]].
    • [3] C. Cutler et al., Phys. Rev. Lett. 70 (1993) 2984 [astro-ph/9208005].
    • [4] P. L. Dufton et al., Astrophys. J. 743 (2011) L22 [arXiv:1111.0157 [astro-ph.SR]].
    • [5] L. Gou, J. E. McClintock, M. J. Reid, J. A. Orosz, J. F. Steiner, R. Narayan, J. Xiang and R. A. Remillard et al., Astrophys. J. 742 (2011) 85 [arXiv:1106.3690 [astro-ph.HE]].
    • [6] J. W. T. Hessels, S. M. Ransom, I. H. Stairs, P. C. C. Freire, V. M. Kaspi and F. Camilo, Science 311 (2006) 1901 [astro-ph/0601337].
    • [7] J. R. Hurley, C. A. Tout and O. R. Pols, Mon. Not. Roy. Astron. Soc. 329 (2002) 897 [astro-ph/0201220].
    • [8] K. R. Lang, Essential Astrophysics, Springer-Verlag, Berlin (2013)
    • [9] C. H. Lee, G. E. Brown and R. A. M. J. Wijers, Astrophys. J. 575 (2002) 996 doi:10.1086/341349 [astroph/0109538].
    • [10] S. E. de Mink, N. Langer, R. G. Izzard, H. Sana and A. de Koter, Astrophys. J. 764 (2013) 166 [arXiv:1211.3742 [astro-ph.SR]].
    • [11] J. E. McClintock et al., Class. Quant. Grav. 28 (2011) 114009 [arXiv:1101.0811 [astro-ph.HE]].
    • [12] E. M. Mendez, MNRAS 413, (2011) 183 arXiv:1011.6385 [astro-ph.HE].
    • [13] E. O'Connor and C. D. Ott, Astrophys. J. 730 (2011) 70 [arXiv:1010.5550 [astro-ph.HE]].
    • [14] R. W. O'Shaughnessy, J. Kaplan, V. Kalogera and K. Belczynski, Astrophys. J. 632 (2005) 1035 [astroph/0503219].
    • [15] S. Privitera et al., Phys. Rev. D 89 (2014) 2, 024003 [arXiv:1310.5633 [gr-qc]].
    • [16] H. Sana, A. de Koter, S. E. de Mink, P. R. Dunstall, C. J. Evans, V. Henault-Brunet, J. M. Apellaniz and O. H. Ramirez-Agudelo et al., arXiv:1209.4638 [astro-ph.SR].
    • [17] S. E. Woosley, Astrophys. J. 405 (1993) 273.
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