GRAVITATIONAL-WAVE TAILS AND BINARY STAR SYSTEMS
GRAVITATIONAL-WAVE TAILS AND BINARY STAR SYSTEMS
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DOI：
10.1088/0264-9381/10/12/026
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发表时间：
1993-12-01
影响因子：
3.5
通讯作者：
SCHAFER, G
中科院分区：
文献类型：
--
作者：
BLANCHET, L;SCHAFER, G
引力波尾是由向外的引力辐射（由孤立系统发射）从与系统总质量相关的弯曲时空反向散射而产生的。本文研究了引力波尾在离系统较远的1.5后牛顿阶波场中的谱（或傅立叶）分解。它示出，波尾的影响是（i）增加的（线性）波的傅立叶分量的振幅的一个因素线性地取决于频率，和（ii）添加到波的相位的补充相位取决于频率为ω ln ω。后一种频率相关的相位引入了一种新的效应，这种效应应该在包含一个以上频率的任何辐射中都可以观察到，例如，在一个以非零偏心率绕开普勒椭圆轨道运行的双星星星系统发出的辐射中，或者在一个螺旋形（紧凑）双星星星系统发出的辐射中。在本文中，我们建议将尾诱导效应（i）和（ii）包括在激光干涉仪引力波探测器（至少在未来，非常敏感，这样的探测器）中的螺旋紧凑的二进制信号的未来数据分析的匹配滤波器中。这样，滤波器将与实际信号高度相关，特别是将保持，作为信号的频率的增加，在准确的相位与it. The波尾的贡献，由一个双星系统发射的总引力能量的计算，和数值应用的脉冲双星PSR 1913+16。我们发现脉冲星轨道P（Th）的尾诱导相对修正为-1.65 × 10 ~（-7）（太小而无法观测到）。
Gravitational wave tails are produced by back-scattering of the outgoing gravitational radiation (emitted by an isolated system) off the curved spacetime associated with the total mass of the system. This paper investigates the spectral (or Fourier) decomposition of gravitational wave tails at large distances from the system, at the 1.5 post-Newtonian order in the wave field. It is shown that the effects of wave tails are (i) to increase the amplitude of the Fourier components of the (linear) waves by a factor linearly depending on the frequency, and (ii) to add to the phase of the waves a supplementary phase depending on the frequency as omega ln omega. The latter frequency-dependent phase introduces a new effect which should be observable in any radiation containing more than one frequency, for instance in the radiation emitted by a binary star system orbiting a Keplerian ellipse with non-zero eccentricity, or in the radiation emitted by an inspiralling (compact) binary star system. We propose in this paper to include the tail-induced effects (i) and (ii) in the matched filters of the future data analysis of inspiralling compact binary signals in laser interferometer gravity-wave detectors (at least in future, very sensitive, such detectors). In this way, the filters will be highly correlated with the actual signal, and in particular will remain, as the frequency of the signal increases, in accurate phase with it. The contribution of the wave tail in the total gravitational energy emitted by a binary system is also calculated, and a numerical application to the binary pulsar PSR 1913+16 is presented. We find that the tail-induced relative correction in the orbital P(Th) of the pulsar is equal to -1.65 x 10(-7) (too small to be observed).