Improving shock irregularities based on the characteristics of the MHD equations
Improving shock irregularities based on the characteristics of the MHD equations
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DOI：
10.1016/j.jcp.2008.05.006
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发表时间：
2008-08
期刊：
影响因子：
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通讯作者：
T. Hanawa;H. Mikami;Tomoaki Matsumoto
中科院分区：
文献类型：
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作者：
T. Hanawa;H. Mikami;Tomoaki Matsumoto
我们开发了一种带有冲击的三维磁流体动力流数值模拟方案。该数值方案基于 Roe 型方案，并包括沿激波锋面切向方向的附加数值扩散，以考虑红宝石的不稳定性。仅在快波或慢波特征收敛的区域（即对红宝石不稳定性有潜在危险的区域）添加数值粘度。因此，除了激波锋面附近之外，数值粘度与 Roe 方案的数值粘度一样小。与HLLE方案的比较表明，我们的方案获得的模拟结果具有更高的磁雷诺数。我们展示了该方案在 II 型超新星磁流体动力学模拟中的应用。还证明了该方案不存在奇偶解耦问题。
We have developed a numerical simulation scheme for three-dimensional magnetohydrodynamical flow with shocks. The numerical scheme is based on the Roe-type scheme and includes additional numerical diffusion in the direction tangential to the shock front to care the carbuncle instability. The numerical viscosity is added only in the regions where the characteristics of either fast or slow wave converges, i.e., in the regions potentially dangerous to the carbuncle instability. Accordingly the numerical viscosity is as small as that of the Roe scheme except near the shock fronts. It is demonstrated from comparison with the HLLE scheme that the magnetic Reynolds number is higher in the simulations obtained with our scheme. We show application of the scheme to the magnetohydrodynamical simulations of type II supernova. It is also proved that the scheme is free from the odd–even decoupling.