  Rapidly rotating, chemically homogeneously evolving massive stars are
considered to be progenitors of long gamma-ray bursts. We present numerical
simulations of the evolution of the circumstellar medium around a rapidly
rotating 20 Msol star at a metallicity of Z=0.001. Its rotation is fast enough
to produce quasi-chemically homogeneous evolution. While conventionally, a star
of 20 Msol would not evolve into a Wolf-Rayet stage, the considered model
evolves from the main sequence directly to the helium main sequence. We use the
time-dependent wind parameters, such as mass loss rate, wind velocity and
rotation-induced wind anisotropy from the evolution model as input for a 2D
hydrodynamical simulation. While the outer edge of the pressure-driven
circumstellar bubble is spherical, the circumstellar medium close to the star
shows strong non-spherical features during and after the periods of
near-critical rotation. We conclude that the circumstellar medium around
rapidly rotating massive stars differs considerably from the surrounding
material of non-rotating stars of similar mass. Multiple blue-shifted high
velocity absorption components in gamma-ray burst afterglow spectra are
predicted. As a consequence of near critical rotation and short stellar
evolution time scales during the last few thousand years of the star's life, we
find a strong deviation of the circumstellar density profile in the polar
direction from the 1/R^2 density profile normally associated with stellar winds
close to the star
