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