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Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-16546

Guedes, J; Diemand, J; Zemp, M; Kuhlen, M; Madeau, P; Mayer, L; Stadel, J (2008). Massive black hole recoil in high resolution hosts. Astronomische Nachrichten, 329(9-10):1004-1007.

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The final inspiral and coalescence of a black hole binary can produce highly beamed gravitational wave radiation. To conserve linear momentum, the black hole remnant can recoil with kick velocity vkick 4000 km/s. We present two sets of full N-body simulations of recoiling massive black holes (MBH) in high-resolution, non-axisymmetric potentials. The host to the first set of simulations is the main halo of the Via Lactea I simulation (Diemand et al. 2007). The nature of the resulting orbits is investigated through a numerical model where orbits are integrated assuming an evolving, triaxial NFWpotential, and dynamical friction is calculated directly from the velocity dispersion along the major axes of the main halo of Via Lactea I. By comparing the triaxial case to a spherical model, we find that the wandering time spent by the MBH is significantly increased due to the asphericity of the halo. For kicks larger than 200 km/s, the remnant MBH does not return to the inner 200 pc within 1 Gyr, a timescale an order of magnitude larger than the upper limit of the estimated QSO lifetime. The second set of simulations is run using the outcome of a high-resolution gas-rich merger (Mayer et al. 2007) as host potential. In this case, a recoil velocity of 500 km/s cannot remove the MBH from the nuclear region. (© 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)


8 citations in Web of Science®
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Additional indexing

Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
Dewey Decimal Classification:530 Physics
Uncontrolled Keywords:black hole physics; gravitational waves; hydrodynamics
Deposited On:26 Feb 2009 15:57
Last Modified:05 Apr 2016 13:06
Funders:NSF Graduate Student Research Fellowship
Additional Information:Published in Astronomische Nachrichten,Volume 329 (2008), Issue 9-10, Pages 1004 - 1007. - The definitive version is available at http://www.interscience.wiley.com/
Publisher DOI:10.1002/asna.200811056
Related URLs:http://arxiv.org/abs/0812.1216
Other Identification Number:ISI:000262794800031

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