10 research outputs found

### Gravitational Recoil of Inspiralling Black-Hole Binaries to Second Post-Newtonian Order

The loss of linear momentum by gravitational radiation and the resulting
gravitational recoil of black-hole binary systems may play an important role in
the growth of massive black holes in early galaxies. We calculate the
gravitational recoil of non-spinning black-hole binaries at the second
post-Newtonian order (2PN) beyond the dominant effect, obtaining, for the first
time, the 1.5PN correction term due to tails of waves and the next 2PN term. We
find that the maximum value of the net recoil experienced by the binary due to
the inspiral phase up to the innermost stable circular orbit (ISCO) is of the
order of 22 km/s. We then estimate the kick velocity accumulated during the
plunge from the ISCO up to the horizon by integrating the momentum flux using
the 2PN formula along a plunge geodesic of the Schwarzschild metric. We find
that the contribution of the plunge dominates over that of the inspiral. For a
mass ratio m_2/m_1=1/8, we estimate a total recoil velocity (due to both
adiabatic and plunge phases) of 100 +/- 20 km/s. For a ratio 0.38, the recoil
is maximum and we estimate it to be 250 +/- 50 km/s. In the limit of small mass
ratio, we estimate V/c to be approximately 0.043 (1 +/- 20%)(m_2/m_1)^2. Our
estimates are consistent with, but span a substantially narrower range than,
those of Favata et al. (2004).Comment: 19 pages, 1 figure, version accepted for publication in The
Astrophysical Journa

### Probing the non-linear structure of general relativity with black hole binaries

Observations of the inspiral of massive binary black holes (BBH) in the Laser
Interferometer Space Antenna (LISA) and stellar mass binary black holes in the
European Gravitational-Wave Observatory (EGO) offer an unique opportunity to
test the non-linear structure of general relativity. For a binary composed of
two non-spinning black holes, the non-linear general relativistic effects
depend only on the masses of the constituents. In a recent letter, we explored
the possibility of a test to determine all the post-Newtonian coefficients in
the gravitational wave-phasing.
However, mutual covariances dilute the effectiveness of such a test. In this
paper, we propose a more powerful test in which the various post-Newtonian
coefficients in the gravitational wave phasing are systematically measured by
treating three of them as independent parameters and demanding their mutual
consistency. LISA (EGO) will observe BBH inspirals with a signal-to-noise ratio
of more than 1000 (100) and thereby test the self-consistency of each of the
nine post-Newtonian coefficients that have so-far been computed, by measuring
the lower order coefficients to a relative accuracy of $\sim 10^{-5}$
(respectively, $\sim 10^{-4}$) and the higher order coefficients to a relative
accuracy in the range $10^{-4}$-0.1 (respectively, $10^{-3}$-1).Comment: 5 pages, 4 figures. Revised version, accepted for publication in
Phys. Rev

### Testing post-Newtonian theory with gravitational wave observations

The Laser Interferometric Space Antenna (LISA) will observe supermassive
black hole binary mergers with amplitude signal-to-noise ratio of several
thousands. We investigate the extent to which such observations afford
high-precision tests of Einstein's gravity. We show that LISA provides a unique
opportunity to probe the non-linear structure of post-Newtonian theory both in
the context of general relativity and its alternatives.Comment: 9 pages, 2 figure

### Inspiralling compact binaries in quasi-elliptical orbits: The complete third post-Newtonian energy flux

The instantaneous contributions to the 3PN gravitational wave luminosity from
the inspiral phase of a binary system of compact objects moving in a quasi
elliptical orbit is computed using the multipolar post-Minkowskian wave
generation formalism. The necessary inputs for this calculation include the 3PN
accurate mass quadrupole moment for general orbits and the mass octupole and
current quadrupole moments at 2PN. Using the recently obtained 3PN
quasi-Keplerian representation of elliptical orbits the flux is averaged over
the binary's orbit. Supplementing this by the important hereditary
contributions arising from tails, tails-of-tails and tails squared terms
calculated in a previous paper, the complete 3PN energy flux is obtained. The
final result presented in this paper would be needed for the construction of
ready-to-use templates for binaries moving on non-circular orbits, a plausible
class of sources not only for the space based detectors like LISA but also for
the ground based ones.Comment: 40 pages. Minor changes in text throughout. Minor typos in Eqs.
(3.3b), (7.7f), (8.19d) and (8.20) corrected. Matches the published versio

### Analytic approximations, perturbation methods, and their applications

The paper summarizes the parallel session B3 {\em Analytic approximations,
perturbation methods, and their applications} of the GR18 conference. The talks
in the session reported notably recent advances in black hole perturbations and
post-Newtonian approximations as applied to sources of gravitational waves.Comment: Summary of the B3 parallel session of the GR18 conferenc

### Summary of Session B3Analytic Approximations, Perturbation Methods and Their Applications

The paper summarizes the parallel session B3 analytic approximations, perturbation methods and their applications of the GR18 conference. The talks in the session reported notably recent advances in black hole perturbations and post-Newtonian approximations as applied to sources of gravitational waves

### Analytic approximations and perturbation methodsand their applications

The paper summarizes the parallel session B3 analytic approximations, perturbation methods and their applications of the GR18 conference. The talks in the session reported notably recent advances in black hole perturbations and
post-Newtonian approximations as applied to sources of gravitational waves