Backflow in simulated MHD accretion disks
arXiv:2012.13194
Abstract
We perform resistive MHD simulations of accretion disk with alpha-viscosity, accreting onto a rotating star endowed with a magnetic dipole. We find backflow in the presence of strong magnetic field and large resistivity, and probe for the dependence on Prandtl number. We find that in the magnetic case the distance from the star at which backflow begins, the stagnation radius, is different than in the hydrodynamic case, and the backflow shows non-stationary behavior. We compare the results with hydrodynamics simulations.
arXiv comment6 pages, 2 figures; to appear in RAGtime22 conference Proceedings
References in corpus (5)
- The PLUTO Code for Adaptive Mesh Computations in Astrophysical Fluid Dynamics
- Strongly magnetized accretion disks: structure and accretion from global magnetohydrodynamic simulations
- Accretion discs around black holes: two dimensional, advection cooled flows
- "Atlas" of numerical solutions for star-disk magnetospheric interaction
- Backflow in Accretion Disk