论文标题
二进制中子星合并残留的检测和参数估计
Detection and parameter estimation of binary neutron star merger remnants
论文作者
论文摘要
二进制中子星合并残留物的检测和参数估计可以阐明近核密度下热物质的物理。在这里，我们开发了一个快速，简单的模型，该模型可以生成重力波形，并证明它可用于检测和参数估计 - 合并后残留物。该模型由三个带有线性频率拖延项的指数抑制正弦曲线组成。模型波形和数值偏移模拟之间的中位拟合因子超过0.90。我们使用贝叶斯因子检测统计量以3000的阈值来检测$ \ ge 7 $的信噪比为$ \ ge 7 $。我们可以将主要后频率限制为$ \ pm_ {1.2}^{1.2}^{1.4}^{1.4} \％$，以达到Mererger sighterger Signal-noise noise in 15的精确率，以达到精确的率。 $ \ pm_ {0.2}^{0.3} \％$的信号 - 噪声比例为50。潮汐耦合常数可以约束至$ \ pm^{9} _ {12} _ {12} \％$，以15和$ \ pm 5的信号为$ \ pm pp pm pp pm pp pm pp pm pp pm pp pm pp pm pp pm pp pp pm pp pm pp pp pm pp pm pp pp pp pm pp pp pp pm farsier推理模型。
Detection and parameter estimation of binary neutron star merger remnants can shed light on the physics of hot matter at supranuclear densities. Here we develop a fast, simple model that can generate gravitational waveforms, and show it can be used for both detection and parameter estimation of post-merger remnants. The model consists of three exponentially-damped sinusoids with a linear frequency-drift term. The median fitting factors between the model waveforms and numerical-relativity simulations exceed 0.90. We detect remnants at a post-merger signal-to-noise ratio of $\ge 7$ using a Bayes-factor detection statistic with a threshold of 3000. We can constrain the primary post-merger frequency to $\pm_{1.2}^{1.4}\%$ at post-merger signal-to-noise ratios of 15 with an increase in precision to $\pm_{0.2}^{0.3}\%$ for post-merger signal-to-noise ratios of 50. The tidal coupling constant can be constrained to $\pm^{9}_{12}\%$ at post-merger signal-to-noise ratios of 15, and $\pm 5\%$ at post-merger signal-to-noise ratios of 50 using a hierarchical inference model.
