  Compression of the stellar winds from rapidly rotating hot stars is described
by the wind compression model. However, it was also shown that rapid rotation
leads to rotational distortion of the stellar surface, resulting in the
appearance of non-radial forces acting against the wind compression. In this
note we justify the wind compression model for moderately rotating white dwarfs
and slowly rotating giants. The former could be conducive to understanding
density/ionization structure of the mass outflow from symbiotic stars and
novae, while the latter can represent an effective mass-transfer mode in the
wide interacting binaries.
