Iteratively comparing gravitational-wave observations to the evolution of massive stellar binaries
Iteratively comparing gravitational-wave observations to the evolution of massive stellar binaries
复制标题
DOI：
10.1103/physrevd.108.043023
复制
发表时间：
2023-03
影响因子：
5
通讯作者：
V. Delfavero;R. O’Shaughnessy;K. Belczynski;Paweł Drozda;D. Wysocki
中科院分区：
文献类型：
--
作者：
V. Delfavero;R. O’Shaughnessy;K. Belczynski;Paweł Drozda;D. Wysocki
引力波观测有能力强烈区分关于致密双星如何形成的不同假设。在这项工作中，我们将展示如何仔细插值的二进制演化模型参数的选择之间的边际似然。使用StarTrack二进制演化代码，我们比较了一维和四维的二进制演化模型，紧凑的二进制合并报告在最近的引力波观测运行。我们首先考虑一个一维模型，研究超新星反冲速度（从麦克斯韦与分散{\sigma}_eff）的影响上的模拟人口的紧凑的二元合并，并找到大量的SN反冲反冲踢的支持。接下来，我们对{\sigma}_eff、质量传递效率（fa）和Roche瓣吸积过程中喷出物质的角动量损耗效率（\B{eta}）进行了四维研究，并根据恒星风模型（fwind 1）估计了观测驱动的质量损失率降低。我们发现，其中三个（{\sigma}_eff，fa和fwind 1）可以有效地限制这些观测比较。在最初从这些参数空间中的均匀先验进行采样后，我们通过迭代估计每个模拟的贝叶斯似然性并将该似然性拟合到参数模型（截断高斯）来改进我们的采样，以便提出新的。我们的最大似然模拟（K 0559）有参数：{\sigma}_eff = 108.3 km/s（表明SN反冲），fa = 0.922（表明有效的质量转移），fwind 1 = 0.328（表明支持减少风驱动的质量损失）。请注意，我们的估计仅在通过孤立双星演化形成致密双星的一个特定模型中有效，尚未考虑其他恒星物理和双星演化的不确定因素的影响。
Gravitational-wave observations have the capability to strongly differentiate between different assumptions for how binary compact objects form. In this work, we show how to carefully interpolate a marginal likelihood between choices of binary evolution model parameters. Using the StarTrack binary evolution code, we compare one- and four-dimensional binary evolution models to the compact binary mergers reported in recent gravitational-wave observing runs. We first consider a one-dimensional model, studying the effect of supernova kick velocity (drawn from a Maxwellian with dispersion {\sigma}_eff) on the simulated population of compact binary mergers, and find support for substantial SN recoil kicks. We follow this up with a four-dimensional study of {\sigma}_eff, mass transfer efficiency (fa) and the efficiency of angular momentum depletion from ejected material (\b{eta}) during Roche-lobe accretion, and an observation-driven reduction in the mass-loss rate estimated from stellar wind models (fwind1). We find that three of them ({\sigma}_eff, fa, and fwind1) can be efficiently limited by these observational comparisons. After initially sampling from a uniform prior in the space of these parameters, we refined our sampling by iteratively estimating a Bayesian likelihood for each simulation and fitting that likelihood to a parametric model (a truncated Gaussian) in order to propose new. Our maximum likelihood simulation (K0559) has parameters: {\sigma}_eff = 108.3 km/s (indicating substantial SN recoil kicks), fa = 0.922 (indicating efficient mass transfer), and fwind1 = 0.328 (indicating support for reduced wind-driven mass loss). Note that our estimates are only valid within one particular model of compact binary formation through isolated binary evolution and do not yet take into account the impact of other uncertain pieces of stellar physics and binary evolution.