Modeling of partly ionized non-equilibrium plasma in the heliosheath: evolution of the solar wind and energetic pariticles toward the heliopause

Details Modeling of partly ionized non-equilibrium plasma in the heliosheath: evolution of the solar wind and energetic pariticles toward the heliopause Modeling of partly ionized non-equilibrium plasma in the heliosheath: evolution of the solar wind and energetic pariticles toward the heliopause

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh11a1911i&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH11A-1911

Physics

[2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2126] Interplanetary Physics / Heliosphere/Interstellar Medium Interactions

Scientific paper

We present first results of a 3D kinetic-MHD numerical model of the solar wind interaction with the local interstellar medium which has been recently advanced by taking into account non-equilibrium local behavior of the velocity distribution function of the charged particles. In this model, all charged particles are divided into several co-moving types. The coldest type, with parameters typical of original solar wind protons, is considered in the framework of fluid approximation. The hot pickup proton components created from interstellar H atoms and heliospheric ENAs by charge exchange are treated kinetically. The charged components are considered self-consistently with interstellar H atoms, which are described kinetically as well. Solar and interstellar magnetic fields are taken into account in the model. Discussion is specifically focused on the evolution of the solar wind and pickup protons in the inner heliosheath from the termination shock to the heliopause. Different aspects of the heliopause structure are discussed as well.

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