**Authors**: Chandra Kant Mishra (RRI & IISc, India), K. G. Arun (CMI, India), Bala R. Iyer (RRI, India)

**Date**: 11 Nov 2011

**Abstract**: Anisotropic emission of gravitational-waves (GWs) from inspiralling compact binaries leads to the loss of linear momentum and hence gravitational recoil of the system. The loss rate of linear momentum in the far-zone of the source (a nonspinning binary system of black holes in quasi-circular orbit) is investigated at the 2.5 post-Newtonian (PN) order and used to provide an analytical expression in harmonic coordinates for the 2.5PN accurate recoil velocity of the binary accumulated in the inspiral phase. The maximum recoil velocity of the binary system at the end of its inspiral phase (i.e at the innermost stable circular orbit (ISCO)) estimated by the 2.5PN formula is of the order of 4 km/s which is smaller than the 2PN estimate of 22 km/s and indicates the importance of higher order post-Newtonian (PN) corrections. Going beyond inspiral, we also provide an estimate of the more important contribution to the recoil velocity from the plunge phase. The maximum recoil velocity at the end of the plunge, involving contributions both from inspiral and plunge phase, for a binary with symmetric mass ratio $\nu=0.2$ is of the order of 182 km/s.

1111.2701
(/preprints)

2011-11-14, 08:27
**[edit]**

© M. Vallisneri 2012 — last modified on 2010/01/29

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