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
Conclusions