  We use high-resolution, three-dimensional hydrodynamic simulations to study
the hydrodynamic and gravitational interaction between stellar companions
embedded within a differentially rotating common envelope. Specifically, we
evaluate the contributions of the nonaxisymmetric gravitational tides and ram
pressure forces to the drag force and, hence, to the dissipation rate and the
mass accumulated onto the stellar companion. We find that the gravitational
drag dominates the hydrodynamic drag during the inspiral phase, leading to the
result that a simple prescription based on a gravitational capture radius
formalism significantly underestimates the dissipation rate and overestimates
the inspiral decay timescale. Although the rate of mass accretion fluctuates
significantly, we observe a secular trend leading to an effective rate of mass
accretion which is significantly less than the rate based on a gravitational
capture radius. The implications of these results are discussed within the
context of accretion of compact objects in the common-envelope phase.
