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Numerical simulations of standing shocks in accretion flows around black holes: A comparative study

机译:黑洞周围吸积物的静冲击冲击的数值模拟:比较研究

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摘要

We compare the results of numerical simulations of thin and quasi-spherical (thick) accretion flows with existing analytical solutions. We use a Lagrangian code based on the smooth particle hydrodynamics (SPH) scheme and an Eulerian finite difference code based on the total variation diminishing (TVD) scheme. In one-dimensional thin flows, the results of the simulations, with or without shocks, agree very well with each other and with analytical solutions. In two-dimensional thick flows, the general features, namely the locations and strengths of centrifugal and turbulent pressure supported shocks, centrifugal barriers, and the funnel walls that are expected from analytical models, agree very well, though the details vary. Generally speaking, the locations of the shocks may be better obtained by SPH since the angular momentum is strictly preserved in SPH, but the shocks themselves are better resolved by TVD. The agreement of these code test results with analytical solutions provides us with confidence to apply these codes to more complex problems, which we will discuss elsewhere
机译:我们将薄和准球形(厚)吸积流的数值模拟结果与现有的解析解进行了比较。我们使用基于光滑粒子流体动力学(SPH)方案的Lagrangian码和基于总变化量递减(TVD)方案的欧拉有限差分码。在一维稀薄流中,无论有无冲击,模拟结果彼此之间以及与解析解上都非常吻合。在二维稠密流动中,一般特征,即离心和湍流压力支撑的冲击的位置和强度,离心屏障以及分析模型所预期的漏斗壁,都可以很好地达成共识,尽管细节有所不同。一般来说,由于SPH严格保留了角动量,因此SPH可能会更好地获得冲击的位置,但是TVD可以更好地解决冲击本身。这些代码测试结果与分析解决方案的协议使我们有信心将这些代码应用于更复杂的问题,我们将在其他地方讨论

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