Gravitational wave peak luminosity model for precessing binary black holes
Gravitational wave peak luminosity model for precessing binary black holes
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DOI：
10.1103/physrevd.102.104047
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发表时间：
2020-09
影响因子：
5
通讯作者：
A. Taylor;V. Varma
中科院分区：
文献类型：
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作者：
A. Taylor;V. Varma
当两个黑洞合并时，在短时间内以引力辐射的形式释放出大量的能量，使此类事件成为宇宙中最明亮的现象之一。预测黑洞合并的峰值亮度的模型是引力波界感兴趣的，在广义相对论的测试中有潜在的应用。我们提出了一个峰值亮度的代理模型，该模型直接在岁差二元黑洞的数值相对论模拟上进行训练。使用高斯过程回归，我们插值的峰值亮度在7维参数空间的旋进双星的质量比为$q\leq4$，和自旋星等为$\chi_1，\chi_2\leq0.8 $。我们表明，我们的估计峰值光度的误差低于现有的拟合公式约一个数量级。此外，我们还建立了一个质量比为q\leq8 $，自旋星等为|\chi_{1z}|,|\chi_{2z}|\leq0.8$.我们应用我们的进动模型来推断GW事件GW 190521的峰值光度，发现结果与以前的预测是一致的。
When two black holes merge, a tremendous amount of energy is released in the form of gravitational radiation in a short span of time, making such events among the most luminous phenomenon in the universe. Models that predict the peak luminosity of black hole mergers are of interest to the gravitational wave community, with potential applications in tests of general relativity. We present a surrogate model for the peak luminosity that is directly trained on numerical relativity simulations of precessing binary black holes. Using Gaussian process regression, we interpolate the peak luminosity in the 7-dimensional parameter space of precessing binaries with mass ratios $q\leq4$, and spin magnitudes $\chi_1,\chi_2\leq0.8$. We demonstrate that our errors in estimating the peak luminosity are lower than those of existing fitting formulae by about an order of magnitude. In addition, we construct a model for the peak luminosity of aligned-spin binaries with mass ratios $q\leq8$, and spin magnitudes $|\chi_{1z}|,|\chi_{2z}|\leq0.8$. We apply our precessing model to infer the peak luminosity of the GW event GW190521, and find the results to be consistent with previous predictions.