Binary Neutron Star Mergers.
Binary Neutron Star Mergers.
复制标题
二进制中子星星合并。
DOI：
10.12942/lrr-2012-8
复制
发表时间：
2012
影响因子：
40.6
通讯作者：
Rasio FA
中科院分区：
文献类型：
--
作者：
Faber JA;Rasio FA
本文综述了双中子星系统聚结的研究现状。我们首先讨论合并双星的形成渠道，并讨论最新的合并率理论预测。接下来，我们转向准平衡公式，这些公式用于在合并阶段之前研究双星并为完全动态模拟生成初始数据。准平衡近似在发展我们对双星合并物理的理解方面发挥了关键作用，特别是对可以驱动双星在寿命结束时合并的轨道不稳定过程的理解。然后我们转向动力学模拟中使用的数值技术，包括相对论形式、(磁流体)动力学、引力波提取技术和核微物理处理。然后是对迄今为止在该领域进行的模拟的总结，包括来自完全相对论和微观物理详细模拟的最新结果。最后，我们讨论了当我们从第一代引力波干涉仪过渡到第二代引力波干涉仪时，以及当超级计算机达到千万亿级前沿时，该领域可能的方向。
We review the current status of studies of the coalescence of binary neutron star systems. We begin with a discussion of the formation channels of merging binaries and we discuss the most recent theoretical predictions for merger rates. Next, we turn to the quasi-equilibrium formalisms that are used to study binaries prior to the merger phase and to generate initial data for fully dynamical simulations. The quasi-equilibrium approximation has played a key role in developing our understanding of the physics of binary coalescence and, in particular, of the orbital instability processes that can drive binaries to merger at the end of their lifetimes. We then turn to the numerical techniques used in dynamical simulations, including relativistic formalisms, (magneto-)hydrodynamics, gravitational-wave extraction techniques, and nuclear microphysics treatments. This is followed by a summary of the simulations performed across the field to date, including the most recent results from both fully relativistic and microphysically detailed simulations. Finally, we discuss the likely directions for the field as we transition from the first to the second generation of gravitational-wave interferometers and while supercomputers reach the petascale frontier.