Towards High-accuracy MHD-Boltzmann Model of the Heliospheric Interface

Details Towards High-accuracy MHD-Boltzmann Model of the Heliospheric Interface Towards High-accuracy MHD-Boltzmann Model of the Heliospheric Interface

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusmsh51a..01b&link_type=abstract

American Geophysical Union, Spring Meeting 2007, abstract #SH51A-01

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2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions, 2151 Neutral Particles (7837)

Scientific paper

With Voyager 1 crossing the solar wind (SW) termination shock and Voyager 2 approaching it, we need to develop highly accurate models of the heliospheric interface capable of reproducing a fine structure of the SW flow in the vicinity of the termination shock (TS) and in the heliosheath. A model of such type should, on the one hand, involve a kinetic treatment of the neutral component in the partially ionized SW and local interstellar medium plasmas and, on the other hand, take advantage of adaptive mesh refinement (AMR) techniques for resolving the heliospheric discontinuities (the TS, the heliopause, the bow shock, and additional transients) sharply enough so that they can be meaningfully compared with the spacecraft observations. Charge exchange between hydrogen atoms and ions substantially modifies the TS shape, its position with respect to the Sun, and, as a consequence, the properties of the SW in the heliosheath. We present new results obtained with our numerical code which models the ion flow magnetohydrodynamically, while transport of neutral hydrogen is described stochastically, using direct simulation Monte Carlo (DSMC) method. Solutions obtained with such calculations are compared with those obtained in the framework of our multi-fluid, AMR model, where different populations of neutral particles are treated hydrodynamically.

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