论文标题
具有不同状态方程的核心偏曲超新星的玻尔兹曼辐射流动力学模拟：核成分的作用和中微子的行为
The Boltzmann-radiation-hydrodynamics Simulations of Core-collapse Supernovae with Different Equations of State: the Role of Nuclear Composition and the Behavior of Neutrinos
论文作者
论文摘要
使用Boltzmann-radiation-Hydrodannicals代码，该代码求解了玻尔兹曼方程进行中微子运输，我们用lattimer and Swesty（LS）以及Furusawa和Furusawa和Shen（FS）的状态核方程（EOSS）介绍了模拟的结果。我们延长了LS模型的模拟时间，并进行了彻底的研究，尽管我们以前的论文简要报道了一些结果。只有LS模型显示了冲击复兴。这似乎源于核成分：不同的核成分会导致光解离的不同能量损失，从而迅速对流和后来中微子驱动的对流的不同强度。在FS模型中看到的原始恒星比在LS模型中更紧凑，因为多核物种的存在使EOS柔和。对于中微子的行为，我们检查了中微子的通量和爱丁顿张量。在光学厚的区域中，中微子的扩散和物质运动的拖动决定了通量。在光学薄的区域中，自由流确定它。将Eddington Tensor与从M1闭合关系获得的张量进行了比较。 M1闭合方案高估了半透明区域中速度依赖性项的贡献。
Using the Boltzmann-radiation-hydrodynamics code, which solves the Boltzmann equation for neutrino transport, we present the results of the simulations with the nuclear equations of state (EOSs) of Lattimer and Swesty (LS) and Furusawa and Shen (FS). We extend the simulation time of the LS model and conduct thorough investigations, though our previous paper briefly reported some of the results. Only the LS model shows the shock revival. This seems to originate from the nuclear composition: the different nuclear composition results in the different energy loss by photodissociation and hence the different strength of the prompt convection and the later neutrino-driven convection. The protoneutron star seen in the FS model is more compact than that in the LS model because the existence of multinuclear species softens the EOS. For the behavior of neutrinos, we examined the flux and the Eddington tensor of neutrinos. In the optically thick region, the diffusion of neutrinos and the dragging by the motion of matter determine the flux. In the optically thin region, the free-streaming determines it. The Eddington tensor is compared with that obtained from the M1-closure relation. The M1-closure scheme overestimates the contribution from the velocity-dependent terms in the semitransparent region.
