NONCLASSICAL VISCOSITY AND RESISTIVITY OF THE SOLAR-WIND PLASMA

In this paper we have estimated typical viscosity and resistivity of t he solar wind using turbulence phenomenology rather than Branskii's [1 965] formalism. Since the solar wind is a collisionless plasma, in thi s paper we have assumed that the dissipation in the solar wind occurs at the proton gyroradius through wave-particle interactions. Using thi s dissipation length scale and the dissipation rates calculated using MHD turbulence phenomenology [Verma et al:, 1995], we estimate the vis cosity and resistivity. The resisitivity has been recalculated using a nomalous scattering time. We find that all of our. transport quantitie s are:several orders of magnitude higher that those calculated using c lassical theories of Branginskii [1965].