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We use a semi-analytic, one-zone model for deeply embedded, massive
accretion disks to make observable predictions for next generation
instruments such as ALMA. We include a self-consistent calculation of the
disk temperature and an approximate treatment of angular momentum transport
via several mechanisms, allowing us to probe non steady-state evolution of
both the star and disk. For massive stars (larger than ~2 solar masses),
gravitational instabilities are the dominant transport mechanism as most of
the mass accumulates, and disk fragmentation is likely. We also examine the
influence of turbulent angular momentum within realistic models for the
collapsing pre-stellar core.
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