Wind-MRI interactions in local models of protoplanetary discs - I. Ohmic resistivity
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Abstract
A magnetic disc wind is an important mechanism that may be responsible for
driving accretion and structure formation in protoplanetary discs. Recent
numerical simulations have shown that these winds can take either the
traditional hourglass' symmetry about the mid-plane, or a
slanted' symmetry
dominated by a mid-plane toroidal field of a single sign. The formation of this
slanted symmetry state has not previously been explained. We use radially local
1D vertical shearing box simulations to assess the importance of large-scale
MRI channel modes in influencing the formation and morphologies of these wind
solutions. We consider only Ohmic resistivity and explore the effect of
different magnetisations, with the mid-plane
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1365-2966
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STFC (ST/T00049X/1)