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