  Although the association of gamma-ray bursts (GRBs) with massive stellar
death is on firm footing, the nature of the progenitor system and the key
ingredients required for a massive star to produce a gamma-ray burst remain
open questions. Here, we investigate the evolution of a massive star with a
closely orbiting compact object companion using the stellar evolution code
MESA. In particular, we examine how the companion influences the angular
momentum and circumstellar environment near the end of the massive star life.
We find that tidal effects can cause the compact object companion to
significantly increase the angular momentum of the massive star, for orbital
periods in the range of up to $\sim 4$ days. We model the density profile
evolution of the massive star and discuss how tidal interactions may also lead
to stripping of the outer stellar envelope in a way that can create an
environment around the binary system that deviates from a typical $1/r^{2}$
wind density profile. We show how our results depend on the metallicity of the
system, initial spin of the star, mass ratio, as well as accretion and dynamo
prescriptions in the simulations. We conclude that these systems may be viable
progenitors for radio-bright, long gamma-ray bursts.
