Renormalized spin coefficients in the accumulated orbital phase for unequal mass black hole binaries

Renormalized 2PN spin contributions to the accumulated orbital phase for LISA sources

We give here a new third post-Newtonisn (3PN) spin-spin contribution (in the PN parameter $ε$) to the accumulated orbital phase of a compact binary, arising from the spin-orbit precessional motion of the spins. In the equal mass case this contribution vanishes, but LISA sources of merging supermassive binary black holes have typically a mass ratio of 1:10. For such non-equal masses this 3PN correction is periodic in time, with period approximately $ε^{-1}$ times larger than the period of gravitational waves. We derive a renormalized and simpler expression of the spin-spin coefficient at 2PN, a…

Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the stars' rotation

We present new (3+1) dimensional numerical relativity simulations of the binary neutron star (BNS) mergers that take into account the NS spins. We consider different spin configurations, aligned or antialigned to the orbital angular momentum, for equal and unequal mass BNS and for two equations of state. All the simulations employ quasiequilibrium circular initial data in the constant rotational velocity approach, i.e. they are consistent with Einstein equations and in hydrodynamical equilibrium. We study the NS rotation effect on the energetics, the gravitational waves (GWs) and on the possib…

Analysis of spin precession in binary black hole systems including quadrupole-monopole interaction

We analyze in detail the spin precession equations in binary black hole systems, when the tidal torque on a Kerr black hole due to quadrupole-monopole coupling is taken into account. We show that completing the precession equations with this term reveals the existence of a conserved quantity at 2PN order when averaging over orbital motion. This quantity allows one to solve the (orbit-averaged) precession equations exactly in the case of equal masses and arbitrary spins, neglecting radiation reaction. For unequal masses, an exact solution does not exist in closed form, but we are still able to …

共振标量场中实时引力波线性响应的紫外结构

Ultraviolet Structure of Real-time Gravitational Wave Linear Response in a Resonant Scalar Field

研究闵氏背景下时变共振标量场中引力波的实时线性响应，利用Schwinger-Keldysh形式发展不等时关联函数的绝热正则化方案，提取单圈响应的紫外结构，并通过局域抵消项实现重整化。

Quasi-circular inspirals and plunges from non-spinning effective-one-body Hamiltonians with gravitational self-force information

The self-force program aims at accurately modeling relativistic two-body systems with a small mass ratio (SMR). In the context of the effective-one-body (EOB) framework, current results from this program can be used to determine the effective metric components at linear order in the mass ratio, resumming post-Newtonian (PN) dynamics around the test-particle limit in the process. It was shown in [Akcay et al., Phys. Rev. D 86 (2012)] that, in the original (standard) EOB gauge, the SMR contribution to the metric component $g^\text{eff}_{tt}$ exhibits a coordinate singularity at the light-ring (L…