  In the course of the life of a massive star, wind-wind interaction can give
rise to the formation of circumstellar nebulae which are both predicted and
observed in the nature. We present generic model calculations to predict the
properties of such nebulae for blue supergiants. From stellar evolution
calculations including rotation, we obtain the time dependence of the stellar
wind properties and of the stellar radiation field. These are used as input for
hydro-calculations of the circumstellar medium throughout the star's life.
Here, we present the results for a rapidly rotating 12 solar masses single
star. This star undergoes a blue loop during its post main sequence evolution,
at the onset of which its contraction spins it up close to critical rotation.
Due to the consequent anisotropic mass loss, the blue supergiant wind sweeps up
the preceding slow wind into an hour glass structure. Its collision with the
previously formed spherical red supergiant wind shell forms a short-lived
luminous nebula consisting of two polar caps and a central inner ring. With
time, the polar caps evolve into mid-latitude rings which gradually move toward
the equatorial plane while the central ring is fading. These structures are
reminiscent to the observed nebulae around the blue supergiant Sher 25 and the
progenitor of SN 1987A. The simple model of an hour glass colliding with a
spherical shell retrieves most of the intriguing nebula geometries discovered
around blue supergiants, and suggests them to form an evolutionary sequence.
Our results indicate that binarity is not required to obtain them.
