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Electric Heating and Angular Momentum Transport in Laminar Models of Protoplanetary Disks

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Observations point toward weak levels of turbulence in protoplanetary disks, and theoretical studies now focus on magneto-thermal winds rather than MRI turbulence as the main driver of mass accretion. Although MHD turbulence might be quenched, large-scale magnetic structures may still transport angular momentum and induce substantial accretion heating inside the disk. Using steady-state radiative MHD models, I examine how much stress and heat can thus be obtained in the weakly ionized parts of protoplanetary disks under the assumption of a purely laminar flow.

This talk is part of the Exoplanet Meetings series.

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