Three-component gasdynamic model for the interaction of the solar wind with the interstellar medium

Details Three-component gasdynamic model for the interaction of the solar wind with the interstellar medium Three-component gasdynamic model for the interaction of the solar wind with the interstellar medium

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982izssr......122b&link_type=abstract

Akademiia Nauk SSSR, Izvestiia, Mekhanika Zhidkosti i Gaza, Sept.-Oct. 1982, p. 122-128. In Russian.

Mathematics

Gas Dynamics, Interstellar Gas, Plasma-Particle Interactions, Solar Wind, Steady Flow, Cosmic Plasma, Hydrogen Atoms, Hydrogen Ions, Mathematical Models, Protons

Scientific paper

The present study investigates the steady flow that results from the interaction of a flow of fully ionized hydrogen from a supersonic three-dimensional source (the solar wind) and a supersonic translational gas flow consisting of electrons, protons, and H atoms (the interstellar wind). The interaction of the solar wind with the charged component of the interstellar wind is described by the Euler gasdynamic equations. It is shown that resonant charge transfer in the region between the shock F (the shock through which passes the interstellar-wind plasma which is decelerated by the solar wind) and the contact surface S (which separates the solar wind from the charged component of the interstellar medium) imparts additional momentum to the charged component of the interstellar wind, insofar as in this region protons are sharply decelerated but H atoms (not experiencing elastic collisions) do not change their velocity. This latter effect leads to the screening of H atoms in the sense of their penetration into the solar system.

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