  We investigate mass ejection from accretion disks formed during the collapse
of rapidly-rotating Wolf-Rayet stars. The neutrino-cooled, black hole (BH)
accretion disk system that forms at the center of the star -- and the ensuing
outflows -- provide the conditions for these systems to be candidate
$r$-process element production sites and potential progenitors of broad-lined
Type Ic (Ic-BL) supernovae. Here we present global, long-term axisymmetric
hydrodynamic simulations of collapsar disks that include angular momentum
transport through shear viscosity, neutrino emission and absorption, a
19-isotope nuclear reaction network and nuclear statistical equilibrium solver,
a pseudo-Newtonian BH with mass and spin modified by accreted matter, and
self-gravity. Starting from a stellar profile collapsed in spherical symmetry,
our models capture disk formation self-consistently, and are evolved until
after the shock wave -- driven by disk winds -- reaches the surface of the
star. None of our models achieve sufficient neutronization to eject significant
amounts of $r$-process elements (detailed nucleosynthesis calculations will
follow in a companion paper). Sufficient $^{56}$Ni is produced to power a
typical type Ic-BL supernova light curve, but the average asymptotic velocity
is a factor $\sim 2-3$ times too slow to account for the typical line widths in
type Ic-BL supernova spectra. The gap in neutrino emission between BH formation
and shocked disk formation, and the magnitude of the subsequent peak in
emission, would be observable diagnostics of the internal conditions of the
progenitor in a galactic collapsar. Periodic oscillations of the shocked disk
prior to its expansion are also a potential observable through their impact on
the the neutrino and gravitational wave signals.
