  Winds of massive stars are an important ingredient in determining their
evolution, final remnant mass, and feedback to the surrounding interstellar
medium. We compare empirical results for OB star winds at low metallicity with
theoretical predictions. Observations suggest very weak winds at SMC
metallicity, but there are exceptions. We identified promising candidates for
rotationally enhanced mass-loss rates with two component wind and partially
stripped stars hiding among OB stars with slow but dense wind in the SMC. A
preliminary analysis of these systems, derived parameters, and their
implications are discussed. Finally, we briefly discuss the interaction of OB
winds near black holes in X-ray binaries.
