Numerics for iles: The ppm compressible gas dynamics scheme
Numerics for iles: The ppm compressible gas dynamics scheme
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iles 的数值：ppm 可压缩气体动力学方案
DOI：
10.1017/9780511618604.007
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发表时间：
2007
期刊：
影响因子：
--
通讯作者：
P. Woodward
中科院分区：
文献类型：
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作者：
P. Woodward
PPM气体动力学方案的发展源于20世纪70年代中期Bram货车Leer对MUSCL方案的早期工作[1-3]。在利弗莫尔，在20世纪70年代末，使用的时刻的内部细胞分布，使MUSCL类似有限元计划被放弃的原因compatibilit与利弗莫尔生产代码。为了重新获得MUSCL的准确性，同时仅使用细胞平均值作为基本数据，PPM，分段抛物线方法，与Phil Colella合作开发[4-7]。在过去的20年里，PPM已经有了很大的发展，以解决[6]和[7]中提出的方案的缺点。PPM还与戴文龙合作扩展到MHD [8-18]，与Karl-Heinz Winkler，Steve Hodson，Norm Zabusky，Jeffrey Pedestrian和Gene Bassett合作广泛应用于射流和超音速剪切层的研究[19-25]，与B合作用于模拟盘状星系中的流动以及静止和运动物体周围的流动[26-28]。Kevin埃德加与大卫波特、Annick Pouquet和Igor Sytine（见本卷后面的文章）合作，广泛应用于对流和湍流问题[29-56]，最近扩展到多流体气体动力学问题。与布鲁斯·弗里克塞尔和卡尔-海因茨·温克勒以及后来的戴文龙合作，也对该方法的隐式版本进行了研究[59-66]。与Dennis Dinge合作，PPM的基于细胞的AMR版本正在开发中[见67]。PPM代码已经在许多并行计算系统上实现，包括一些具有数千个处理器的系统[68-69; 54-55]。PPM气体动力学方案的版本已经被纳入3个针对天体物理应用的社区代码：FLASH [参考文献]，ENZO [参考文献]和VH-1 [参考文献]。由于文献中对1984年或1986年版本PPM的几个改进和修改尚未发表，我们在这里从头到尾列出了简单，单流体，理想气体动力学的本方案。然后简要回顾了立方周期区域中均匀、各向同性、可压缩湍流的部分结果。
The development of the PPM gas dynamics scheme grew out of earlier work in the mid 1970s with Bram van Leer on the MUSCL scheme [1-3]. At Livermore, in the late 1970s, the use of moments of the internal cell distributions which makes MUSCL resemble finite element schemes was abandoned for reasons of compatibilit with Livermore production codes. In order to recapture the accuracy of MUSCL while using only cell averages as the fundamental data, PPM, the Piecewise-Parabolic Method, was developed in collaboration with Phil Colella [4-7]. Over the last 20 years, PPM has evolved considerably in order to address shortcomings of the scheme as it was laid out in [6] and [7]. PPM has also been extended to MHD [8-18] in collaboration with Wenlong Dai, applied extensively to the study of jets and supersonic shear layers [19-25] in collaboration with Karl-Heinz Winkler, Steve Hodson, Norm Zabusky, Jeffrey Pedelty, and Gene Bassett, used to simulate flow in disk galaxies and around stationary and moving objects [26-28] in collaboration with B. Kevin Edgar, applied extensively to convection and turbulence problems [29-56] in collaboration with David Porter, Annick Pouquet, and Igor Sytine (see later article in this volume), and most recently extended to multifluid gas dynamics problems. Implicit versions of the method have also been worked on [59-66] in collaboration with Bruce Fryxell and Karl-Heinz Winkler and, later, Wenlong Dai. A cell-based AMR version of PPM has been under development [see 67], in collaboration with Dennis Dinge. The PPM code has been implemented on many parallel computing systems, including some with thousands of processors [68-69; 54-55]. Versions of the PPM gas dynamics scheme have become incorporated into 3 community codes aimed at astrophysics applications: FLASH [refs], ENZO [refs], and VH-1 [refs].Because the several improvements and modifications to the 1984 or 1986 versions of PPM in the literature have not been published, we here lay out the present scheme for simple, single-fluid, ideal gas dynamics from start to finish. Then selected results on homogeneous, isotropic, compressible turbulence in a cubical, periodic domain are briefly reviewed.