Kinetic vs. multi-fluid approach for interstellar neutrals in the heliosphere: exploration of the interstellar magnetic field effects

Details Kinetic vs. multi-fluid approach for interstellar neutrals in the heliosphere: exploration of the interstellar magnetic field effects Kinetic vs. multi-fluid approach for interstellar neutrals in the heliosphere: exploration of the interstellar magnetic field effects

2011-03-16

arxiv.org/abs/1103.3202v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

submitted to Astrophysical Journal

Scientific paper

We present a new 3d self-consistent two-component (plasma and neutral hydrogen) model of the solar wind interaction with the local interstellar medium (LISM). This model (K-MHD) combines the MHD treatment of the solar wind and the ionized LISM component, with a kinetic model of neutral interstellar hydrogen (LISH). The local interstellar magnetic field (BLISM) intensity and orientation are chosen based on an early analysis of the heliosheath flows (Opher et al. 2009). The properties of the plasma and neutrals obtained using the (K-MHD) model are compared to previous multi-fluid (Opher et al. 2009) and kinetic models (Izmodenov et al. 2005). The new treatment of LISH revealed important changes in the heliospheric properties not captures by the multi-fluid model. These include a decrease in the heliocentric distance to the termination shock (TS), a thinner heliosheath and a reduced deflection angle ({\theta}) of the heliosheath flows. The asymmetry of the termination shock, however, seems to be unchanged by the kinetic aspect of the LISH.

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