The effects of nonlinear fluctuations due to solar wind streams upon radial gradients of average solar wind parameters are computed by using a numerical MHD model for both spherically symmetric time-dependent and corotating equatorial flow approximations. We find significant effects of correlations between fluctuations upon the gradients of azimuthal magnetic field, radial velocity, density, and azimuthal velocity. The averages of Vr and r2n both decrease with increasing radial distance (0--30 km/s, 5--10% by 6 AU) while mass flux is conserved. The cross-variance between Vr and r2n increases with radial distance from negative values to positive values at distances greater than 3.5 AU. The average azimuthal velocity decreases, and at distances greater than 4 AU it may be opposite to the solar rotation: ⟨Vϕ⟩ of from 0.2 to -1.7 km/s at 6 AU is predicted. Between 400 and 900 Rs, stream interactions have transferred the major portion of the angular momentum flux to the magnetic field; at even greater distances the plasma again carries the bulk of the angular momentum flux. The average azimuthal component of the magnetic field may decrease as much as 10% faster than the Archimedean spiral out to 6 AU, owing to stream interactions, but this result is dependent upon inner boundary conditions.