Magnetohydrodynamic convection in accretion discs
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Peer-reviewed
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Abstract
Convection has been discussed in the field of accretion discs for several
decades, both as a means of angular momentum transport and also because of its
role in controlling discs' vertical structure via heat transport. If the gas is
sufficiently ionized and threaded by a weak magnetic field, convection might
interact in non-trivial ways with the magnetorotational instability (MRI).
Recently, vertically stratified local simulations of the MRI have reported
considerable variation in the angular momentum transport, as measured by the
stress to thermal pressure ratio
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1365-2966