二维和三维中碰撞恒星和脉冲星风的轨道演化;维度、EoS、分辨率和网格尺寸的影响
Orbital evolution of colliding star and pulsar winds in 2D and 3D; effects of: dimensionality, EoS, resolution, and grid size
摘要：
双星中一颗大质量恒星和一颗非吸积脉冲星的激波所形成的结构会受到轨道和非线性动力学起源的周期性和随机变化的影响。第一次，我们模拟了三维各向同性恒星和相对论脉冲星风的相互作用，沿着1个完整的轨道，尺度远远超过了二进制的大小。我们还研究了网格分辨率和大小的影响，以及不同的EOO：一个伽马常数的理想气体，和一个理想气体与伽马依赖于温度。我们进行了，与代码PLUTO，相对论HD模拟在2和3 D的相互作用的慢风和相对论风与伽玛=2沿1个完整的轨道高达~100 x的二进制大小。不同的2-D模拟进行了相同的和更大的网格分辨率和大小，其中一个是用一个更现实的状态方程，比在3 D。三维模拟证实了以前二维模拟的结果.在三维中，激波流的不稳定性增长更快，这增强了激波、混合和大尺度扰动的存在。在2D中，更高分辨率的模拟证实了更低分辨率的结果，更大网格尺寸的模拟强化了冲击风结构失去全局一致性的情况，并且使用2种不同EoO的模拟产生了非常相似的结果。除了KHI，我们发现，Richtmyer-Meshkov和RTI很可能是共同作用的冲击流的演变。三维模拟证实，恒星风和脉冲星风的相互作用产生了非线性演化和强烈纠缠的结构。这种演变伴随着强烈的动能耗散、流向和速度的快速变化以及湍流运动。结果加强的情况下，大尺度上的冲击结构的全球一致性的损失，虽然更高的脉冲星风速模拟是必要的。
英文摘要：
(abridged)The structure formed by the shocked winds of a massive star and a non-accreting pulsar in a binary suffers periodic and random variations of orbital and non-linear dynamical origin. For the 1st time, we simulate in 3 D the interaction of isotropic stellar and relativistic pulsar winds along 1 full orbit, on scales well beyond the binary size. We also investigate the impact of grid resolution and size, and of different EoOs: a gamma-constant ideal gas, and an ideal gas with gamma dependent on temperature. We carry out, with the code PLUTO, relativistic HD simulations in 2 and 3 D of the interaction of a slow wind and a relativistic wind with Gamma=2 along 1 full orbit up to ~100 x the binary size. The different 2-D simulations are carried out with equal and larger grid resolution and size, and 1 of them is done with a more realistic equation of state, than in 3 D. The simulations in 3 D confirm previous results in 2 D. The shocked flows are subject to a faster instabilities growth in 3 D, which enhances the presence of shocks, mixing, and large-scale disruption. In 2 D, higher resolution simulations confirm lower resolution results, simulations with larger grid sizes strengthen the case for the loss of global coherence of the shocked-wind structure, and simulations with 2 different EoOs yield very similar results. In addition to the KHI, we find that the Richtmyer-Meshkov and the RTI are likely acting together in the shocked flow evolution. Simulations in 3 D confirm that the interaction of stellar and pulsar winds yields structures that evolve non-linearly and get strongly entangled. The evolution is accompanied by strong kinetic energy dissipation, rapid changes in flow orientation and speed, and turbulent motion. The results strengthen the case for the loss of global coherence of the shocked structure on large scales, although higher pulsar wind speed simulations are needed.
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