  Bianchi I cosmological models consisting of a fluid with both bulk and shear
viscosity are studied. It is shown how the dynamical importance of the shear
and the fluid density change in the course of evolution. Exact solutions with
an equation of state $\rho = p$ for a stiff fluid are also obtained in several
special cases, assuming the viscosity coefficients to be the power functions of
the density. The results are, in some relevant cases, compared with those of
Belinskii and Khalatnikov (1976) in the asymptotic limits and are seen to agree
with them in that the models start with $\rho = 0$ at the beginning and evolve
with the creation of matter by the gravitational field, finally approaching the
Friedmann universe.
