Systematic effects from black hole-neutron star waveform model uncertainties on the neutron star equation of state
Systematic effects from black hole-neutron star waveform model uncertainties on the neutron star equation of state
复制标题
黑洞-中子星波形模型不确定性对中子星状态方程的系统影响
DOI：
10.1103/physrevd.99.024049
复制
发表时间：
2019
影响因子：
5
通讯作者：
Lackey, Benjamin D.
中科院分区：
文献类型：
--
作者：
Chakravarti, Kabir;Gupta, Anuradha;Bose, Sukanta;Duez, Matthew D.;Caro, Jesus;Brege, Wyatt;Foucart, Francois;Ghosh, Shaon;Kyutoku, Koutarou;Lackey, Benjamin D.
我们确定了各种贡献者的系统性影响的中子星星（NS）潮汐变形的测量和量化的几种类型的中子星黑洞（NSBH）双星的幅度。来自NSBH合并的引力波包含了关于组分质量和自旋以及NS状态方程的信息。提取这些信息需要将有噪声的探测器数据中的信号与从后牛顿（PN）近似、有效单体（EOB）模型和数值相对论（NR）模拟的某种组合中导出的理论模板进行比较。这些模板的准确性受到NR模拟中的误差、PN/EOB波形的近似性质以及用于联合收割机组合它们的混合过程的限制。在本文中，我们估计这些错误的影响，通过构建和比较一组PN-NR混合波形，第一次与NR波形从两个不同的代码，即SpECandsacra，这样的系统。然后，我们试图恢复的二进制usingtwononon-precessing模板逼近的参数。正如预期的那样，这些误差对可探测性的影响可以忽略不计。质量和自旋的估计受到系统误差的影响，而恢复的质量可能是不准确的，在更高的质量比。大的不确定性也被发现在潮汐变形性，由于在PN基础模型中使用的杂交，数值相对论NR错误的差异，和杂交方法的固有局限性。我们发现，系统误差太大的潮汐效应准确地描述任何现实的NS状态方程模型。我们的结论是，NSBH波形模型必须显着改善，如果他们是有用的NS状态方程信息的提取，甚至区分NSBH系统从二元黑洞。
We identify various contributors of systematic effects in the measurement of the neutron star (NS) tidal deformability and quantify their magnitude for several types of neutron star—black hole (NSBH) binaries. Gravitational waves from NSBH mergers contain information about the components’ masses and spins as well as the NS equation of state. Extracting this information requires comparison of the signal in noisy detector data with theoretical templates derived from some combination of post-Newtonian (PN) approximants, effective one-body (EOB) models, and numerical relativity (NR) simulations. The accuracy of these templates is limited by errors in the NR simulations, by the approximate nature of the PN/EOB waveforms, and by the hybridization procedure used to combine them. In this paper, we estimate the impact of these errors by constructing and comparing a set of PN-NR hybrid waveforms, for the first time with NR waveforms from two different codes, namely,SpECandsacra, for such systems. We then attempt to recover the parameters of the binary usingtwonon-precessing template approximants. As expected, these errors have negligible effect on detectability. Mass and spin estimates are moderately affected by systematic errors for near equal-mass binaries, while the recovered masses can be inaccurate at higher mass ratios. Large uncertainties are also found in the tidal deformability, due to differences in PN base models used in hybridization, numerical relativity NR errors, and inherent limitations of the hybridization method. We find that systematic errors are too large for tidal effects to be accurately characterized for any realistic NS equation of state model. We conclude that NSBH waveform models must be significantly improved if they are to be useful for the extraction of NS equation of state information or even for distinguishing NSBH systems from binary black holes.
登录
查看更多内容
双中子星与 Whiskey 和 SACRA 的合并：独立广义相对论流体动力学代码结果的首次定量比较
影响因子：
5
作者：
L. Baiotti;M. Shibata;Tetsuro Yamamoto
通讯作者：
Tetsuro Yamamoto
影响因子：
3.5
作者：
I. Hinder;A. Buonanno;M. Boyle;Z. Etienne;J. Healy;N. Johnson-McDaniel;A. Nagar;H. Nakano;
通讯作者：
I. Hinder;A. Buonanno;M. Boyle;Z. Etienne;J. Healy;N. Johnson-McDaniel;A. Nagar;H. Nakano;
使用高级 LIGO 测量中子星潮汐变形：中子星-黑洞双星观测的贝叶斯分析
DOI：
--
发表时间：
2016
期刊：
影响因子：
--
作者：
Prayush Kumar;M. Purrer;H. Pfeiffer
通讯作者：
H. Pfeiffer
DOI：
--
发表时间：
2009
期刊：
影响因子：
--
作者：
M. Boyle;Abdul H. Mrou'e
通讯作者：
Abdul H. Mrou'e
后牛顿/数值相对论混合波形对引力波探测器的适用性
影响因子：
3.5
作者：
I. MacDonald;S. Nissanke;H. Pfeiffer
通讯作者：
H. Pfeiffer