中子星模拟的体粘滞系数公式
Formulating bulk viscosity for neutron star simulations
摘要：
为了从强大的中子星合并事件中提取编码在引力和电磁信号中的精确物理信息，我们需要在数值模拟中包括尽可能多的相关物理。这提出了一个严峻的挑战，因为许多涉及的参数约束不足。在本文中，我们集中在核反应的作用。结合理论讨论与分析连接到国家的最先进的模拟，我们概述了多个参数，导致反应系统被描述的体积粘度。结果表明，为了正确地考虑核反应，未来的模拟必须能够处理不同的制度，而不同的假设/近似是适当的。我们还触及到的链接模型的基础上，大涡捕捉湍流所需的战略。
英文摘要：
In order to extract the precise physical information encoded in the gravitational and electromagnetic signals from powerful neutron-star merger events, we need to include as much of the relevant physics as possible in our numerical simulations. This presents a severe challenge, given that many of the involved parameters are poorly constrained. In this paper we focus on the role of nuclear reactions. Combining a theoretical discussion with an analysis connecting to state-of-the-art simulations, we outline multiple arguments that lead to a reactive system being described in terms of a bulk viscosity. The results demonstrate that in order to properly account for nuclear reactions, future simulations must be able to handle different regimes where rather different assumptions/approximations are appropriate. We also touch upon the link to models based on the large-eddy-strategy required to capture turbulence.
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