Fig. 9
Comparison of simulated galaxy properties with MRI conditions from Korpi (2010): MRI damping curve (see Eq. (13)) for fiducial model (dashed line) and expected growth rate of the MRI Ωm (see Eq. (14)) at different times (solid lines). MRI is predicted to be damped by gas random motions in the regions where the solid line is above the dashed line.
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