  We present results of simulations to assess the feasibility of modeling
outflows from massive stars using the Los Alamos 3-D radiation hydrodynamics
code Cassio developed for inertial confinement fusion (ICF) applications. We
find that a 1-D stellar envelope simulation relaxes into hydrostatic
equilibrium using computing resources that would make the simulation tractable
in 2-D. We summarize next steps to include more physics fidelity and model the
response to a large and abrupt energy deposition at the base of the envelope.
