• There is a variety of
line profile morphologies seen in Chandra
observations of massive stars, indicating that a surprising variety of high-energy
physical processes are occurring in this class of stars.
•Normal massive stars with strong
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
•Any time instrumentation improves
significantly, surprising
discoveries will be made