Residual eccentricity of inspiralling orbits at the gravitational-wave detection threshold: Accurate estimates using post-Newtonian theory
Residual eccentricity of inspiralling orbits at the gravitational-wave detection threshold: Accurate estimates using post-Newtonian theory
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引力波探测阈值处螺旋轨道的残余偏心率：使用后牛顿理论的准确估计
DOI：
10.1103/physrevd.104.104023
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发表时间：
2021
影响因子：
5
通讯作者：
Will, Clifford M.
中科院分区：
文献类型：
--
作者：
Tucker, Alexandria;Will, Clifford M.
我们使用包含引力辐射反应项的运动方程，通过4.5后牛顿阶来计算非旋转致密体的吸气二元系统的晚时偏心率，因为它们越过了地基引力波干涉仪的检测阈值。初始偏心率可以大到0.999。我们发现，最终的偏心率是系统小于领先的四极近似预测的，由高达30%的300太阳质量的二进制跨越LIGO/处女座检测阈值在10赫兹，或百分之八小60太阳质量的二进制。我们找到了一个精确解释高阶后牛顿效应的晚期偏心率的解析公式，推广了彼得斯和马修斯在20世纪60年代推导的公式。我们还发现，最终的偏心率是独立的两个致密体的质量比优于百分之二。
We use equations of motion containing gravitational radiation-reaction terms through 4.5 post-Newtonian order to calculate the late-time eccentricities of inspiralling binary systems of nonspinning compact bodies as they cross the detection threshold of ground-based gravitational-wave interferometers. The initial eccentricities can be as large as 0.999. We find that the final eccentricities are systematically smaller than those predicted by the leading quadrupole approximation, by as much as 30 percent for a 300 solar mass binary crossing the LIGO/Virgo detection threshold at 10 Hz, or eight percent smaller for a 60 solar mass binary. We find an analytic formula for the late-time eccentricity that accurately accounts for the higher-order post-Newtonian effects, generalizing a formula derived by Peters and Mathews in the 1960s. We also find that the final eccentricities are independent of the ratio of the masses of the two compact bodies to better than two percent.
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影响因子：
3.5
作者：
B. Moore;N. Yunes
通讯作者：
B. Moore;N. Yunes
广义相对论中的近心推进：后牛顿高阶方法的比较
影响因子：
3.5
作者：
Alexandria Tucker;C. Will
通讯作者：
C. Will
DOI：
10.3847/1538-4357/aaafce
发表时间：
2017-06
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Bao-Minh Hoang;S. Naoz;B. Kocsis;F. Rasio;F. Dosopoulou
通讯作者：
Bao-Minh Hoang;S. Naoz;B. Kocsis;F. Rasio;F. Dosopoulou
从偏心致密双星到 2PN 精度的全解析频域引力波形式
影响因子：
2.4
作者：
M. Tessmer;Gerhard Schaefer
通讯作者：
Gerhard Schaefer