The Origins of Protostellar Core Angular Momenta
  We present the results of a suite of numerical simulations designed to
explore the origin of the angular momenta of protostellar cores. Using the
hydrodynamic grid code \emph{Athena} with a sink implementation, we follow the
formation of protostellar cores and protostars (sinks) from the subvirial
collapse of molecular clouds on larger scales to investigate the range and
relative distribution of core properties. We find that the core angular momenta
are relatively unaffected by large-scale rotation of the parent cloud; instead,
we infer that angular momenta are mainly imparted by torques between
neighboring mass concentrations and exhibit a log-normal distribution. Our
current simulation results are limited to size scales $\sim 0.05$~pc ($\sim
10^4 \rm AU$), but serve as first steps toward the ultimate goal of providing
initial conditions for higher-resolution studies of core collapse to form
protoplanetary disks.
