Outline
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
Much of the work in this talk was done by Swarthmore students, Roban Kramer and Stephanie Tonnesen