Speaker
Description
Backflow is a part of the flow in the accretion disk which is directed away from the star. Although it is well established in purely hydro-dynamical framework, it is only recently that it has been identified in magnetohydrodynamics (MHD) simulations. We perform resistive magnetohydrodynamics (MHD) simulations of an accretion disk with alpha-viscosity, accreting onto a slowly rotating star endowed with a magnetic dipole. We find backflow in the disk-midplane for a range of conditions when the Prandtl number is less than a critical value. Close to the critical Prandtl number value the backflow shows non-stationary behavior. We compare the results with hydrodynamics simulations. We find that in the MHD case the distance from the star at which backflow begins, the stagnation radius, is different than in the hydrodynamic case.
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