Systematic bias on parametrized tests of general relativity due to neglect of orbital eccentricity
Systematic bias on parametrized tests of general relativity due to neglect of orbital eccentricity
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DOI：
10.1103/physrevd.106.084031
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发表时间：
2022-03
影响因子：
5
通讯作者：
P. Saini;Marc Favata;K. Arun
中科院分区：
文献类型：
--
作者：
P. Saini;Marc Favata;K. Arun
引力波观测提供了一个独特的机会来测试广义相对论（GR）在强场和高度动态的理论。GR的参数化测试是一种众所周知的方法，用于量化违反GR。这种方法约束后牛顿定相公式的系数偏差，该公式描述了一个紧凑的二元引力波相位演化，因为它的吸气。使用LIGO/Virgo观测的测试的当前边界假设二进制在它们进入探测器频带时被循环。在这里，我们研究了剩余二元偏心率对参数化测试的影响。我们研究的系统偏差的参数界时，定相的基础上的圆形轨道假设是一个系统，有一些小的剩余偏心率。我们发现，一个系统的偏差（例如，在领先的牛顿变形参数）变得可比的统计误差，即使是中等偏心率的$\sim 0.04$在10 $赫兹的LIGO/处女座带的二元黑洞，和$\sim 0.008$的二元中子星。这种情况发生在第三代（3G）探测器（如宇宙探测器）频带中更低的轨道偏心率值（对于双黑洞，$\sim 0.005$在$10$ Hz，对于双中子星，$\sim 0.002$）。这些结果表明，将偏心率等物理效应纳入波形模型对于从未来探测器中准确提取科学结果非常重要。
Gravitational-wave observations provide a unique opportunity to test general relativity (GR) in the strong-field and highly dynamical regime of the theory. Parametrized tests of GR are one well-known approach for quantifying violations of GR. This approach constrains deviations in the coefficients of the post-Newtonian phasing formula, which describes the gravitational-wave phase evolution of a compact binary as it inspirals. Current bounds from this test using LIGO/Virgo observations assume that binaries are circularized by the time they enter the detector frequency band. Here, we investigate the impact of residual binary eccentricity on the parametrized tests. We study the systematic biases in the parameter bounds when a phasing based on the circular orbit assumption is employed for a system that has some small residual eccentricity. We find that a systematic bias (for example, on the leading Newtonian deformation parameter) becomes comparable to the statistical errors for even moderate eccentricities of $\sim 0.04$ at $10$ Hz in LIGO/Virgo band for binary black holes, and $\sim 0.008$ for binary neutron stars. This happens at even lower values of orbital eccentricity in the frequency band of third-generation (3G) detectors like Cosmic Explorer ($\sim 0.005$ at $10$ Hz for binary black holes and $\sim 0.002$ for binary neutron stars). These results demonstrate that incorporating physical effects like eccentricity in waveform models is important for accurately extracting science results from future detectors.