  In this paper, we discuss some consequences of rotation and mass loss on the
evolved stages of massive star evolution. The physical reasons of the time
evolution of the surface velocity are explained, and then we show how the
late-time evolution of massive stars are impacted in combination with the
effects of mass loss. The most interesting result is that in some cases, a
massive star can have a blue-red-blue evolution, opening the possibility that
Blue Supergiants are composed by two distinct populations of stars: one just
leaving the main sequence and crossing the HRD for the first time, and the
other one evolving back to the blue side of the HRD after a Red Supergiant
phase. We discuss a few possible observational tests that can allow to
distinguish these two populations, and how supergiant B[e] stars fit in this
context.
