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Paper: MHD Heating in Dusty Proto-Stellar Accretion Disks Midplane
Volume: 464, Circumstellar Dynamics at High Resolution
Page: 365
Authors: Jatenco-Pereira, V.
Abstract: A minimum amount of ionization in proto-stellar accretion disks is necessary for the magneto-rotational instability (MRI) to take place, leading to accretion of material towards the central star. As proto-stellar disks are composed of dust, in this work we consider the damping of Alfvén waves due to dust-cyclotron resonances as an additional heating mechanism to viscous accretion disks. When charged grains become coupled to the waves, they introduce a cutoff (resonance) in the Alfvén wave spectrum, providing an important damping mechanism for the waves. Here, we show that the damping of the waves can increase the temperature of the disk, resulting in an increase on the ionization fraction, thus reducing the extension of quiescent zones in the disk.
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