On the distribution function of H atoms in the problem of the solar wind interaction with the local interstellar medium

Details On the distribution function of H atoms in the problem of the solar wind interaction with the local interstellar medium On the distribution function of H atoms in the problem of the solar wind interaction with the local interstellar medium

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998jgr...103.9575b&link_type=abstract

Journal of Geophysical Research, Volume 103, Issue A5, p. 9575-9586

Physics

58

Interplanetary Physics: Heliopause And Solar Wind Termination, Interplanetary Physics: Interstellar Gas, Interplanetary Physics: Neutral Particles, Interplanetary Physics: Solar Wind Plasma

Scientific paper

This paper is devoted to the analysis of the models of the solar wind interaction with the local interstellar medium (LISM) self-consistently taking into account mutual influence of plasma (electrons and protons) and neutral (H atoms) components of the LISM. The axisymmetric interaction model of Baranov and Malama [1993], that used the kinetic description of H atoms motion together with the hydrodynamic approximation for the plasma component, showed that the distribution functions of the all H atom populations are essentially not Maxwellian. The hydrodynamic model by Zank et al. [1996] is based on the Maxwellian distribution functions of the LISM and solar wind hydrogen atoms. The comparisons of the results obtained on the basis of the kinetic model by Baranov and Malama [1993] and multifluid model by Zank et al. [1996] show that the distributions of H atom parameters have large quantitative as well as qualitative distinctions. A number of theoretical predictions and relevant, experimental data are analyzed.

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