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

Part of the Space Sciences Series of ISSI book series (SSSI, volume 31)

Abstract

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.

Keywords

Heliosphere Solar wind Interstellar gas Termination shock Heliopause Heliosheath Bow shock Charge exchange Magnetic field 

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Copyright information

© Springer Science+Business Media, BV 2008

Authors and Affiliations

  1. 1.Department of Mechanics and Mathematics, Institute for Problem in Mechanics, Moscow State UniversityRussian Academy of SciencesMoscowRussia

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