Numerical MHD codes for modeling astrophysical flows |
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| Institution: | 1. Moscow Institute of Physics and Technology, Dolgoprudnyy, Moscow region 141700, Russia;3. Keldysh Institute of Applied Mathematics RAS, Miusskaya sq., 4, Moscow 125047, Russia;4. Department of Astronomy, Cornell University, Ithaca, NY 14853, United States;5. Department of Physics, Cornell University, Ithaca, NY 14853, United States;6. Department of Applied and Eng. Physics, Cornell University, Ithaca, NY 14853, United States;1. Department of Physics and Astronomy, Butler University, Indianapolis, IN 46208, USA;2. College of Science/Department of Physics & NAOC-GZU-Sponsored Center for Astronomy Research, Guizhou University, Guiyang 550025, PR China;3. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, PR China;1. School of Studies in Physics, Jiwaji University, Gwalior 474011, India;2. Greater Noida Institute of Technology, Plot No. 7, Knowledge Park-II, Greater Noida 201306, India;3. Department of Physics, Lovely Professional University, Phagwara 144411, India;4. Zentrum für Astronomie und Astrophysik, Technische Universität Berlin, Hardenbergstrasse 36, D-10623 Berlin, Germany;1. Department of Physics, Indian Institute of Technology Ropar, Nangal Road, Rupnagar 140001, Punjab, India;2. Raman Research Institute, C.V. Raman Avenue, Sadashivanagar, Bangalore 560012, India;3. INAF/IASF-Bologna, via Gobetti 101, I-40129 Bologna, Italy;4. Laboratoire AIM, CEA-IRFU/CNRS/Universit e Paris Diderot, Service d’Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France |
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| Abstract: | 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. |
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