The magneto-rotational instability (MRI) is believed to be the mechanism responsible for a magneto-hydrodynamic (MHD) turbulence that could lead to the accretion observed in proto-stellar accretion disks. A minimum amount of ionization in this medium is necessary for the MRI to take place. In this work we study the role of MHD waves as an additional source of heating in disks. As dust is present in this medium, we suggest that the Alfven waves are damped by the dust-cyclotron mechanism of damping. We present a disk model with two heating mechanisms: the "anomalous" viscosity considered in terms of the α-parameterization and the damping of Alfven waves. We show that the waves can increase the temperature of the disk and can reduce the quiescent region.
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