There is a relatively wide variety of line
profile morphologies seen in Chandra and XMM
observations of OB stars, indicating that a surprising variety of
high-energy physical processes are occurring in early-type
stars
Supergiants with massive radiation-driven winds
have X-ray emitting plasma distributed throughout their
winds: Standard wind-shock models explain the data if the
mean optical depth of the cool wind component is several
times lower than expected (mass-loss rates overestimated?
clumping?)
Young O and early B stars are well explained by
the hybrid magnetically channeled wind shock model
Normal B stars dont fit neatly into any of these
paradigms