Introduction:
the context of hot star X-rays
Line
profile diagnostics
What
do the observations look like?
What
trends emerge?
z
Pup: wind X-rays, but less absorption than expected
z Ori and d Ori: similar situation,
very little wind absorption; but wind-shock
parameters are otherwise satisfactory
Magnetic OB stars are a
different story: q1 Ori C, t
Sco, g Cas
And so are normal B stars: b Cru, e
CMa
Conclusions