Introduction: the context of hot star X-rays
What do the observations look like?
What trends emerge, and how can the properties of the individual stars and of the trends among lines and among stars be explained by the physical effects we expect might be present?
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
Binaries and other types of hot stars
Prospects for the future