Shock waves in the presence of charge exchange: MHD-kinetic modeling

Details Shock waves in the presence of charge exchange: MHD-kinetic modeling Shock waves in the presence of charge exchange: MHD-kinetic modeling

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh53b1499b&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH53B-1499

Other

2109 Discontinuities (7811), 2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions, 2134 Interplanetary Magnetic Fields, 2151 Neutral Particles (7837)

Scientific paper

From a gas dynamic perspective, the interaction of the solar wind (SW) with the local interstellar medium (LISM) is essentially a combination of jet and blunt-body flows. The SW flow is supersonic and super-Alfvénic, while the LISM flow is supersonic, but possibly sub-Alfvénic, if the intensity of the interstellar magnetic field is larger than commonly expected. Thus, the interaction pattern should include both a bow shock ahead of the heliopause and a solar wind termination shock. Since LISM plasma is only partially ionized, the density of neutral hydrogen being possibly 3--4 times greater than that of hydrogen ions, one would expect that charge exchange can modify the structure of these shocks in some way. On the other hand, the mean free path of neutral particles with respect to charge exchange with plasma particles is larger than the characteristic scale of the problem. This means that a physically justified approach to model their transport should be based on solving the Boltzmann equation. We developed a self-consistent MHD-neutral model of the heliospheric interface that is based on the high- resolution, shock-capturing methods and adaptive mesh refinement technique for shocked plasma and Monte Carlo simulation for neutral particles. We apply a one-dimensional version of this model to investigate the influence of charge exchange on the bow shock structure and flow parameters on its high-pressure side. Both slow- and fast-mode configurations are considered.

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