  In this paper we have estimated typical anomalous viscosity, resistivity, and
thermal difffusivity of the solar wind plasma. Since the solar wind is
collsionless plasma, we have assumed that the dissipation in the solar wind
occurs at proton gyro radius through wave-particle interactions. Using this
dissipation length-scale and the dissipation rates calculated using MHD
turbulence phenomenology [{\it Verma et al.}, 1995a], we estimate the viscosity
and proton thermal diffusivity. The resistivity and electron's thermal
diffusivity have also been estimated. We find that all our transport quantities
are several orders of magnitude higher than those calculated earlier using
classical transport theories of {\it Braginskii}. In this paper we have also
estimated the eddy turbulent viscosity.
