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MRI channel flows in accretion disks

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If you have a question about this talk, please contact Dr Geoffroy Lesur .

Local simulations of magnetorotational instability (MRI) in non-stratified and stratified accretion disks sometimes exhibit recurrent coherent structures called channel flows. The formation and destruction of these structures may play a role in the development and saturation of MRI -induced turbulence, and consequently help us understand the time-dependent accretion behaviour of certain astrophysical objects. In this talk I will discuss the properties of channel flows and the secondary parasitic instabilities to which they are subject.

This talk is part of the DAMTP Astrophysics Seminars series.

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