Numerical MHD Codes for Modeling Astrophysical Flows
arXiv:1508.00003 · doi:10.1016/j.newast.2015.10.011
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.
23 pages, 17 figures, submitted to New Astronomy
References in corpus (4)
Cited by in corpus (6)
- Properties of Strong and Weak Propellers from MHD Simulations
- Evolution of the Magnetized, Neutrino-Cooled Accretion Disk in the Aftermath of a Black Hole Neutron Star Binary Merger
- 3D Simulations of Planet Trapping at Disc-Cavity Boundaries
- The effects of a magnetic field on planetary migration in laminar and turbulent discs
- Eccentricity Growth of Massive Planets inside Cavities of Protoplanetary Discs
- Comparisons of MHD Propeller Model with Observations of Cataclysmic Variable AE Aqr