Self-consistent model of the solar wind interaction with three-component circumsolar interstellar cloud: Mutual influence of thermal plasma, galacticcosmic rays, and H atoms

In this paper we continue our study of the galactic cosmic ray (GCR) influe nce on the structure of the heliospheric interface plasma flow [Myasnikov e t al., this issue]. The model presented here is more realistic and takes th e mutual influence of plasma, neutral, and cosmic ray components into accou nt self-consistently. In the model, GCRs are described hydrodynamically und er the assumption that their mass density is negligible; while neutrals are described kinetically. We explore the GCR influence on the heliospheric in terface plasma structure by varying the diffusion coefficient, cosmic ray p ressure, and adiabatic index. The problem is studied numerically, using the global iterations that couple the soft fitting technique for describing th e plasma and GCR components and Monte Carlo simulations for H atoms. A stro ng GCR modulation is found in the heliospheric interface. At the same time, the GCR influence on the plasma flow is negligible as compared with the in fluence of H atoms. The exception is the bow shock, a structure which can b e strongly modified by the cosmic rays. The Baranov-Malama model is therefo re acceptable for interpretation of the physical processes in the heliosphe re as long as the processes are not related to the bow shock structure. Alt hough the simplest model of the cosmic ray transport is good enough to esti mate GCR influence on the plasma and atom distributions in the heliospheric interface, more advanced models should be used to interpret the observed G CR spectra.