How reliable are MRI simulations? The role of the magnetic Prandtl number
Duration: 1 hour 1 min
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About this item
| Description: |
Fromang, S (CEA/Saclay)
Wednesday 30 September 2009, 09:30-10:30 |
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| Created: | 2009-10-09 18:08 | ||
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| Collection: | Dynamics of Discs and Planets | ||
| Publisher: | Isaac Newton Institute | ||
| Copyright: | Fromang, S | ||
| Language: | eng (English) | ||
| Credits: |
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| Abstract: | Thanks to high resolution local simulations, the last few years have seen significant progresses in our understanding of MHD turbulence driven by the magnetorotational instability. Small scale explicit dissipation coefficients (viscosity and resistivity), traditionnally excluded from such simulations in the past, have been shown to be extremely important to set the saturated amplitude of the turbulence. In this talk I will review these recent results and discuss their consequences for protoplanetary disks structure and planet formation theories. |
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