Testing the post-Newtonian expansion with GW170817
Testing the post-Newtonian expansion with GW170817
复制标题
使用 GW170817 测试后牛顿展开式
DOI：
10.1007/s10714-023-03100-z
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发表时间：
2021
影响因子：
2.8
通讯作者：
C. Capano
中科院分区：
文献类型：
--
作者：
Andrey A. Shoom;Pawan Kumar Gupta;B. Krishnan;A. Nielsen;C. Capano
对致密双星合并产生的引力波的观测使得在动力学和非线性领域对广义相对论进行独特的测试成为可能。最重要的此类测试之一是对引力波信号相位的后牛顿（PN）校正的约束。 PN 系数的值可以在标准广义相对论中计算，并且这些值在许多替代引力理论中是不同的。显然，基于引力波观测来限制偏差非常有意义。在大多数已进行的且产生迄今为止最严格约束的此类测试中，通常单独改变这些 PN 系数。虽然原则上这可能有助于检测与标准广义相对论的某些偏差，但它是一个严重的限制。例如，我们期望重力的替代理论通常具有附加参数。对 PN 系数的修正预计将取决于这些额外的非 GR 参数，因此，我们预计各种 PN 系数高度相关。我们在这里使用来自双中子星聚结 GW170817 的数据提出了另一种分析。我们的分析使用非 GR 参数的适当线性组合，这些参数表示与 TaylorF2 近似相中相应的后牛顿螺旋系数的绝对偏差。这些组合表示不相关的非 GR 参数，这些参数对应于参数子空间中协方差矩阵的主方向。我们的结果表明与 GR 非常一致。特别是，积分非 GR 相位为 $$\Psi _{{\tiny int-non-GR}} = 0.0447\pm 25.3000$$ Ψ i n t - n o n - G R = 0.0447 ± 25.3000，与 GR 百分位数的偏差为 $$p^{{\tiny Dev-GR}}_{n}=25.85\%$$ p n Dev - G R = 25.85 % 。
Observations of gravitational waves from compact binary mergers have enabled unique tests of general relativity in the dynamical and non-linear regimes. One of the most important such tests is constraints on the post-Newtonian (PN) corrections to the phase of the gravitational wave signal. The values of the PN coefficients can be calculated within standard general relativity, and these values are different in many alternate theories of gravity. It is clearly of great interest to constrain the deviations based on gravitational wave observations. In the majority of such tests which have been carried out, and which yield by far the most stringent constraints, it is common to vary these PN coefficients individually. While this might in principle be useful for detecting certain deviations from standard general relativity, it is a serious limitation. For example, we would expect alternate theories of gravity to generically have additional parameters. The corrections to the PN coefficients would be expected to depend on these additional non-GR parameters, whence, we expect that the various PN coefficients to be highly correlated. We present an alternate analysis here using data from the binary neutron star coalescence GW170817. Our analysis uses an appropriate linear combination of non-GR parameters that represent absolute deviations from the corresponding post-Newtonian inspiral coefficients in the TaylorF2 approximant phase. These combinations represent uncorrelated non-GR parameters which correspond to principal directions of their covariance matrix in the parameter subspace. Our results illustrate good agreement with GR. In particular, the integral non-GR phase is $$\Psi _{{\tiny int-non-GR}} = 0.0447\pm 25.3000$$ Ψ i n t - n o n - G R = 0.0447 ± 25.3000 and the deviation from GR percentile is $$p^{{\tiny Dev-GR}}_{n}=25.85\%$$ p n D e v - G R = 25.85 % .
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影响因子：
5
作者：
J. Blackman;Scott E. Field;M. Scheel;C. Galley;C. Ott;M. Boyle;Lawrence E. Kidder;H. Pfeiffer;B. Szil'agyi
通讯作者：
J. Blackman;Scott E. Field;M. Scheel;C. Galley;C. Ott;M. Boyle;Lawrence E. Kidder;H. Pfeiffer;B. Szil'agyi
DOI：
10.3847/1538-4357/ab0108
发表时间：
2018-11
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Nitz;C. Capano;A. Nielsen;S. Reyes;R. White;Duncan A. Brown;B. Krishnan
通讯作者：
A. Nitz;C. Capano;A. Nielsen;S. Reyes;R. White;Duncan A. Brown;B. Krishnan
影响因子：
8.6
作者：
Abbott, B. P.;Abbott, R.;Zweizig, J.
通讯作者：
Zweizig, J.
使用主成分分析对后牛顿理论进行参数化检验
影响因子：
5
作者：
Saleem, M.;Datta, Sayantani;Arun, K. G.;Sathyaprakash, B. S.
通讯作者：
Sathyaprakash, B. S.