Achamveedu Gopakumar

Comparison between numerical-relativity and post-Newtonian waveforms from spinning binaries : The orbital hang-up case

We compare results from numerical simulations of spinning binaries in the ‘‘orbital hang-up’’ case, where the binary completes at least nine orbits before merger, with post-Newtonian results using the approximants Taylor T1, T4, and Et. We find that, over the ten cycles before the gravitational-wave frequency reaches M! ¼ 0:1, the accumulated phase disagreement between numerical relativity (NR) and 2.5 post-Newtonian (PN) results is less than three radians, and is less than 2.5 radians when using 3.5PN results. The amplitude disagreement between NR and restricted PN results increases with the black holes’ spin, from about 6% in the equal-mass case to 12% when the black holes’ spins are Si=M 2 ¼ 0:85. Finally, our results suggest that the merger waveform will play an important role in estimating the spin from such inspiral waveforms.

Gravitational recoil during binary black hole coalescence using the effective one body approach

During the coalescence of binary black holes, gravitational waves carry linear momentum away from the source, which results in the recoil of the center of mass. Using the effective one body approach, which includes nonperturbative resummed estimates for the damping and conservative parts of the compact binary dynamics, we compute the recoil during the late inspiral and the subsequent plunge of nonspinning black holes of comparable masses moving in quasicircular orbits. Further, using a prescription that smoothly connects the plunge phase to a perturbed single black hole, we obtain an estimate for the total recoil associated with the binary black hole coalescence. We show that the crucial physical feature which determines the magnitude of the terminal recoil is the presence of a burst of linear-momentum flux emitted slightly before coalescence. When using the most natural expression for the linear-momentum flux during the plunge, together with a Taylor-expanded

MEASURING THE SPIN OF THE PRIMARY BLACK HOLE IN OJ287

(v/c{)}^{4}

Third post-Newtonian accurate generalized quasi-Keplerian parametrization for compact binaries in eccentric orbits

correction factor, we find that the maximum value of the terminal recoil is

Post-Newtonian accurate parametric solution to the dynamics of spinning compact binaries in eccentric orbits: The leading order spin-orbit interaction

ensuremath{sim}74text{ }text{ }mathrm{km}/mathrm{s}

Phasing of gravitational waves from inspiralling eccentric binaries

and occurs for

Comparison between numerical relativity and a new class of post-Newtonian gravitational-wave phase evolutions: The nonspinning equal-mass case

ensuremath{eta}=({m}_{1}{m}_{2})/({m}_{1}+{m}_{2}{)}^{2}ensuremath{simeq}0.2

Phasing of gravitational waves from inspiralling eccentric binaries at the third-and-a-half post-Newtonian order

, i.e., for a mass ratio

Deterministic nature of conservative post-Newtonian accurate dynamics of compact binaries with leading order spin-orbit interaction

{m}_{2}/{m}_{1}ensuremath{simeq}0.38

Frequency and time domain inspiral templates for comparable mass compact binaries in eccentric orbits

. Away from this optimal mass ratio, the recoil velocity decreases approximately proportionally to the scaling function