Other
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21460504l&link_type=abstract
American Astronomical Society, AAS Meeting #214, #605.04
Other
Scientific paper
In models of disk accretion driven by the magnetorotational instability (MRI) mass flow in protoplanetary disks is not uniform throughout all disk heights, but is instead concentrated in the layers of the disk away from the midplane (Gammie 1996). It is not common in radiative transfer models to consider such "layered accretion.” We have developed a 1.5D simulation to solve for a protoplanetary disk's temperature profile following the algorithm of Dullemond et al. (2002). This method imposes hydrostatic equilibrium and uses radiative transfer to iteratively find a temperature solution. To this method we have added a viscous heating term q = (9/4)ρνΩ2 where the viscosity ν we assume is a parameterized "α-viscosity” as described in Shakura-Sunyaev (1973). We have tested a range of α values in two cases: One where the mass accretion is uniform through all disk heights, and another where the mass accretion is concentrated in the outer layers of the disk with a "dead zone” imposed elsewhere (α=0). We find that even when considering the same mass flow through a disk, the temperature profiles differ between the uniform accretion and layered accretion cases. Further results will be presented.
Desch Steven J.
Lesniak Michael V. III
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