Backflow in simulated MHD accretion disks. (arXiv:2012.13194v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mishra_R/0/1/0/all/0/1">Ruchi Mishra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cemeljic_M/0/1/0/all/0/1">Miljenko Čemeljić</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kluzniak_W/0/1/0/all/0/1">Wlodek Kluźniak</a>
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.
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.
http://arxiv.org/icons/sfx.gif
