The early evolution of viscous and self-gravitating circumstellar disks
  with a dust component
  The long-term evolution of a circumstellar disk starting from its formation
and ending in the T Tauri phase was simulated numerically with the purpose of
studying the evolution of dust in the disk with distinct values of viscous
\alpha-parameter and dust fragmentation velocity v_frag. We solved numerical
hydrodynamics equations in the thin-disk limit, which are modified to include a
dust component consisting of two parts: sub-micron-sized dust and grown dust
with a maximum radius a_r. The former is strictly coupled to the gas, while the
latter interacts with the gas via friction. The conversion of small to grown
dust, dust growth, and dust self-gravity are also considered. We found that the
process of dust growth known for the older protoplanetary phase also holds for
the embedded phase of disk evolution. The dust growth efficiency depends on the
radial distance from the star - a_r is largest in the inner disk and gradually
declines with radial distance. In the inner disk, a_r is limited by the dust
fragmentation barrier. The process of small-to-grown dust conversion is very
fast once the disk is formed. The total mass of grown dust in the disk (beyond
1 AU) reaches tens or even hundreds of Earth masses already in the embedded
phase of star formation and even a greater amount of grown dust drifts in the
inner, unresolved 1 AU of the disk. Dust does not usually grow to radii greater
than a few cm. A notable exception are models with \alpha <= 10^{-3}, in which
case a zone with reduced mass transport develops in the inner disk and dust can
grow to meter-sized boulders in the inner 10 AU. Grown dust drifts inward and
accumulates in the inner disk regions. This effect is most pronounced in the
\alpha <= 10^{-3} models where several hundreds of Earth masses can be
accumulated in a narrow region of several AU from the star by the end of
embedded phase. (abridged).
