We use a semi-analytic, one-zone model for deeply embedded 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 stars larger than ~1 solar mass, gravitational
instabilities are the dominant transport mechanism as most of the mass
accumulates, and for stars more than twice this mass, 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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