  We describe X-ray production in the atmospheres of hot, early-type stars in
the framework of a ``stochastic shock model''. The extended envelope of a star
is assumed to possess numerous X-ray emitting ``hot'' zones that are produced
by shocks and embedded in the ambient ``cold'' medium in dynamical equilibrium.
It is shown that the apparent lack of X-ray variability on short (order of
hours) timescales do not contradict a shock model for X-ray production. The
character of the X-ray variability is found to depend on the frequency with
which hot zones are generated, the cool wind opacity to X-rays, and the wind
flow parameters, such as mass loss rate and terminal speed.
