标题： 引力波探测器中紧凑双星旋进信号的后牛顿模板比较 显示英文标题

标题： Comparison of post-Newtonian templates for compact binary inspiral signals in gravitational-wave detectors

摘要： 在广义相对论中，两体动力学已通过后牛顿（PN）近似进行微扰求解。轨道相位的演化和发出的引力辐射现在已知到相当高的阶数，达到O(v^8)，其中v是双星系统的特征速度。然而，由于在PN展开中选择参数的固有自由度以及求解相关微分方程的方法不同，轨道演化无法唯一确定。本文的目标是在初始和先进的引力波探测器的背景下，确定不同PN波形族之间的（不）一致程度。我们分析中使用的波形是目前初始LIGO/Virgo所使用的，即时域PN模型TaylorT1、TaylorT2、TaylorT3、TaylorT4和TaylorEt，有效单体（EOB）模型，以及频域表示TaylorF2。我们检查这些模型彼此之间以及与原型有效单体模型（校准到数值相对论模拟，如目前初始LIGO所使用的）在2PN、3PN和3.5PN阶数下的重叠情况，以量化它们的差异，并帮助我们决定是否存在作为搜索模板最合适的家族。我们得出结论，只要总质量保持在某个上限M_crit以下，所有3.5PN阶数的模板家族（除TaylorT3和TaylorEt外）对于检测目的都是同样有效的。M_crit的值被发现约为12M_Sun对于初始、增强和先进的LIGO。从纯粹计算的角度来看，我们建议在Mcrit以下使用3.5PN TaylorF2，在总双星质量M > Mcrit时使用校准到数值相对论模拟的EOB。 显示英文摘要

摘要： The two-body dynamics in general relativity has been solved perturbatively using the post-Newtonian (PN) approximation. The evolution of the orbital phase and the emitted gravitational radiation are now known to a rather high order up to O(v^8), v being the characteristic velocity of the binary. The orbital evolution, however, cannot be specified uniquely due to the inherent freedom in the choice of parameter used in the PN expansion as well as the method pursued in solving the relevant differential equations. The goal of this paper is to determine the (dis)agreement between different PN waveform families in the context of initial and advanced gravitational-wave detectors. The waveforms employed in our analysis are those that are currently used by Initial LIGO/Virgo, that is the time-domain PN models TaylorT1, TaylorT2, TaylorT3, TaylorT4 and TaylorEt, the effective one-body (EOB) model, and the Fourier-domain representation TaylorF2. We examine the overlaps of these models with one another and with the prototype effective one-body model (calibrated to numerical relativity simulations, as currently used by initial LIGO) for a number of different binaries at 2PN, 3PN and 3.5PN orders to quantify their differences and to help us decide whether there exist preferred families that are the most appropriate as search templates. We conclude that as long as the total mass remains less than a certain upper limit M_crit, all template families at 3.5PN order (except TaylorT3 and TaylorEt) are equally good for the purpose of detection. The value of M_crit is found to be ~ 12M_Sun for Initial, Enhanced and Advanced LIGO. From a purely computational point of view we recommend that 3.5PN TaylorF2 be used below Mcrit and EOB calibrated to numerical relativity simulations be used for total binary mass M > Mcrit.