Kinetic-Fluid Perspective on Modeling the Heliospheric/Interstellar Medium Interface

Details Kinetic-Fluid Perspective on Modeling the Heliospheric/Interstellar Medium Interface Kinetic-Fluid Perspective on Modeling the Heliospheric/Interstellar Medium Interface

Mar 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009ssrv..143..449b&link_type=abstract

Space Science Reviews, Volume 143, Issue 1-4, pp. 449-464

Physics

4

Heliosphere, Solar Wind, Interstellar Gas, Termination Shock, Heliopause, Heliosheath, Bow Shock, Charge Exchange, Magnetic Field

Scientific paper

Content of the invited paper for Workshop “From the Outer Heliosphere to the Local Bubble: Comparison of New Observations with Theory” organized by International Space Science Institute (ISSI) is presented. Main results of the kinetic-fluid model of the solar wind interaction with the partially ionized supersonic flow of the local interstellar medium (LISM) by Baranov and Malama (J. Geophys. Res. 98(A9):15,157-15,163, 1993) and its development by Moscow group to take into account effects of solar cycles, cosmic rays, non-equilibrium processes, magnetic field and so on are given. It is shown that multi-fluid models are not correct for problem considered due to Knudsen number Kn= l ch / L˜1, where l ch is the mean free path of H atoms for collisions connected with the resonance charge exchange, L is the characteristic length of the problem. Important problems connected with the physical properties of the heliospheric boundary and with magnetohydrodynamics (MHD) of the solar wind interaction with the LISM are discussed.

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