Kinetic-Gasdynamic Modeling of the Heliospheric Interface

Details Kinetic-Gasdynamic Modeling of the Heliospheric Interface Kinetic-Gasdynamic Modeling of the Heliospheric Interface

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009ssrv..146..329i&link_type=abstract

Space Science Reviews, Volume 146, Issue 1-4, pp. 329-351

Physics

22

Inner Heliosheath, Interstellar H Atoms, Heliospheric Ena

Scientific paper

Heliospheric energetic neutral atoms (ENAs) that will be measured by the Interstellar Boundary Explorer (IBEX) originate from the heliosheath. The heliosheath is formed as a result of the interaction of the solar wind (SW) with the circum-heliospheric interstellar medium (CHISM). The expected fluxes of ENAs are strongly dependent on the nature of this interaction. In turn, the interaction of the solar wind with the local interstellar cloud has a complex and multi-component nature. Detailed theoretical modeling of the interaction between the SW and the local interstellar medium is required to understand the physics of the heliosheath and to predict and explain the heliospheric ENAs. This paper summarizes current state-of-art kinetic-gasdynamic models of the SW/CHISM interaction. We shall restrict our discussion to the kinetic-gasdynamic and kinetic-magnetohydrodynamic (MHD) models developed by the Moscow group. This paper summarizes briefly the main results of the first self-consistent, two-component, kinetic-gasdynamic model by Baranov and Malama (J. Geophys. Res. 98:15157-15163, 1993), presents new results obtained from the 3D kinetic-MHD model by Izmodenov et al. (Astron. Astrophys. 437:L35-L38, 2005a), describes the basic formulation and results of the model by Malama et al. (Astron. Astrophys. 445:693-701, 2006) as well as reports current developments in the model. This self-consistent model considers pickup protons as a separate non-equilibrium component. Then we discuss a stochastic acceleration model for pickup protons in the supersonic solar wind and in the heliosheath. We also present the expected heliospheric ENA fluxes obtained in the framework of the models.

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