Numerical MHD codes for modeling astrophysical flows

被引：9

作者：

Koldoba, A. V. ^{[1
,2
]}

Ustyugova, G. V. ^{[3
]}

Lii, P. S. ^{[4
]}

Comins, M. L. ^{[4
]}

Dyda, S. ^{[5
]}

Romanova, M. M. ^{[4
]}

Lovelace, R. V. E. ^{[4
,6
]}

机构：

[1] Moscow Inst Phys & Technol, Dolgoprudnyy 141700, Moscow Region, Russia

[2] Inst Comp Aided Design RAS, 2nd Brestskaya St,19-18, Moscow 123056, Russia

[3] Keldysh Inst Appl Math RAS, Miusskaya Sq 4, Moscow 125047, Russia

[4] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA

[5] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA

[6] Cornell Univ, Dept Appl & Engn Phys, Ithaca, NY 14853 USA

来源：

NEW ASTRONOMY | 2016年 / 45卷

基金：

美国国家科学基金会;

关键词：

Numerical methods; Codes; Magnetohydrodynamics; APPROXIMATE RIEMANN SOLVER; RADIATION MAGNETOHYDRODYNAMICS CODE; 2 SPACE DIMENSIONS; ALGORITHMS; SCHEMES; SYSTEMS; ZEUS-2D; ATHENA;

D O I：

10.1016/j.newast.2015.10.011

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We describe a Godunov-type magnetohydrodynamic (MHD) code based on the Miyoshi and Kusano (2005) solver which can be used to solve various astrophysical hydrodynamic and MHD problems. The energy equation is in the form of entropy conservation. The code has been implemented on several different coordinate systems: 2.5D axisymmetric cylindrical coordinates, 2D Cartesian coordinates, 2D plane polar coordinates, and fully 3D cylindrical coordinates. Viscosity and diffusivity are implemented in the code to control the accretion rate in the disk and the rate of penetration of the disk matter through the magnetic field lines. The code has been utilized for the numerical investigations of a number of different astrophysical problems, several examples of which are shown. (C) 2015 Elsevier B.V. All rights reserved.

引用

页码：60 / 76

页数：17

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