论文标题
受核物理学，观测和QCD计算的新的状态方程
New equations of state constrained by nuclear physics, observations, and QCD calculations of high-density nuclear matter
论文作者
论文摘要
我们提出了用于核心崩溃超新星和中子星合并模拟中应用的新状态方程。我们首先引入有效的质量参数化，该参数适合最近的微观计算，最高两倍的饱和密度。这对于捕获预测的热效应很重要，这些效应已证明可以确定超新星模拟中的原始中子恒星收缩。核密度方程的能量密度函数的参数范围受到核密度的手性有效现场理论结果，以及基于QCD的高密度下的功能重新规范化组计算。我们进一步通过测量重中子恒星，GW170817的重力波信号以及最近的更好结果来实现观察性约束。最后，我们研究了所得允许的状态方程和中子恒星特性的范围，包括中子恒星半径和最大质量的预测范围。
We present new equations of state for applications in core-collapse supernova and neutron star merger simulations. We start by introducing an effective mass parametrization that is fit to recent microscopic calculations up to twice saturation density. This is important to capture the predicted thermal effects, which have been shown to determine the proto-neutron star contraction in supernova simulations. The parameter range of the energy-density functional underlying the equation of state is constrained by chiral effective field theory results at nuclear densities as well as by functional renormalization group computations at high densities based on QCD. We further implement observational constraints from measurements of heavy neutron stars, the gravitational wave signal of GW170817, and from the recent NICER results. Finally, we study the resulting allowed ranges for the equation of state and for properties of neutron stars, including the predicted ranges for the neutron star radius and maximum mass.
