1995/09/05 by Mahendra K. Verma, Verma, Mahendra K.
Physics and Astronomy · #Astro and Planetary Science #Chaotic Dynamics (nlin.CD) #FOS: Physical sciences #Ionosphere and magnetosphere dynamics #Solar and Space Plasma Dynamics
paper · pdf · doi:10.48550/arxiv.chao-dyn/9509002
openalex publication_date 1995/09/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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.