  Several topics in the theory of magnetized turbulence are reviewed with
application to star formation and the interstellar medium. The density,
pressure, and temperature distribution in a turbulent interstellar medium is
described in comparison to a medium dominated by thermal instability. The
derivation of the empirical theory for the energy spectrum of hydrodynamic and
MHD turbulence is outlined, and comparisons are given to numerical models for
the magnetized case. Next discussed is how density fluctuations modify
observations of velocity fluctuations in line centroids, coincidentally
cancelling the effects of projection smoothing. The analytic description of
velocity structure functions as a function of the dimensionality of the
dissipative structures is then covered. Finally the question of whether
turbulence can support against gravitational collapse is addressed. Turbulence
both prevents and promotes collapse, but its net effect is to inhibit collapse,
so it does not trigger star formation in any significant sense.
