Reliability of complete gravitational waveform models for compact binary coalescences
Reliability of complete gravitational waveform models for compact binary coalescences
复制标题
紧凑二元合并完整引力波形模型的可靠性
DOI：
10.1103/physrevd.84.064029
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发表时间：
2011
影响因子：
5
通讯作者：
S. Husa
中科院分区：
文献类型：
--
作者：
F. Ohme;M. Hannam;S. Husa
准确的知识引力波（GW）信号从吸入紧凑双星是
这对于在GW干涉仪的数据中检测这些特征是必不可少的。随着近年来的发展，
牛顿（PN）理论和数值相对论（NR），
通过将这两种描述组合成一个完整的混合信号来产生波形。同时解决
这种波形在物理参数空间的不同点的可靠性，以前的研究
确定PN贡献为主要误差源，可以通过结合
长NR模拟。在本文中，我们克服了两个突出的问题，使其难以
确定为GW产生适当精确的混合所需的最小模拟长度
天文学应用：（1）GW搜索的相关标准是真实
波形和一组模型波形，对模型中的所有波形进行了优化，但对于离散波形，
混合动力车这种优化是不可能的。(2)这些计算通常需要
波形已经存在，而我们开发了一种算法来估计混合失配误差，
数值数据，这使我们能够在执行前估计必要的NR波形长度。
仿真我们的程序依赖于在最高可用的组合假定等效PN模型
顺序与NR制度中的常见数据，它们的差异作为不确定性的度量
假设在每个波形中。与一些早期的研究相反，我们估计，10 NR轨道之前，
合并应该允许构造足够精确的波形族，以用于在
广泛的参数范围，仅排除高度旋转，不等质量的系统。非旋转系统，
即使具有高质量比（q * 20），也很好地模拟了天体物理学上合理的组件质量。在
此外，总质量和对称质量比的参数偏差仅为1%或更小
小于0.1的无量纲自旋幅度。我们认为，类似的NR波形长度将
保持先进探测器时代的技术水平，并开始评估科学的局限性，
都可以用它们来完成。
Accurate knowledge of the gravitational-wave (GW) signal from inspiraling compact binaries is
essential to detect these signatures in the data from GW interferometers. With recent advances in post-
Newtonian (PN) theory and numerical relativity (NR) it has become possible to construct inspiral-mergerringdown
waveforms by combining both descriptions into one complete hybrid signal. While addressing
the reliability of such waveforms in different points of the physical parameter space, previous studies have
identified the PN contribution as the dominant source of error, which can be reduced by incorporating
longer NR simulations. In this paper we overcome the two outstanding issues that make it difficult to
determine the minimum simulation length necessary to produce suitably accurate hybrids for GW
astronomy applications: (1) the relevant criteria for a GW search is the mismatch between the true
waveform and a set of model waveforms, optimized over all waveforms in the model, but for discrete
hybrids this optimization was not yet possible. (2) these calculations typically require that numerical
waveforms already exist, while we develop an algorithm to estimate hybrid mismatch errors without
numerical data, which enables us to estimate the necessary NR waveform length before performing the
simulation. Our procedure relies on combining supposedly equivalent PN models at highest available
order with common data in the NR regime, and their difference serves as a measure of the uncertainty
assumed in each waveform. Contrary to some earlier studies, we estimate that �10 NR orbits before
merger should allow for the construction of waveform families that are accurate enough for detection in a
broad range of parameters, only excluding highly spinning, unequal-mass systems. Nonspinning systems,
even with high mass-ratio (q * 20) are well modeled for astrophysically reasonable component masses. In
addition, the parameter bias is only of the order of 1% for total mass and symmetric mass-ratio and less
than 0.1 for the dimensionless spin magnitude. We take the view that similar NR waveform lengths will
remain the state of the art in the advanced detector era, and begin to assess the limits of the science that
can be done with them.
影响因子：
8.6
作者：
Ajith, P.;Hannam, M.;Seiler, J.
通讯作者：
Seiler, J.