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Cite abstracts as Author(s) (2005), Title, Eos Trans. AGU,
86
(52), Fall Meet. Suppl., Abstract xxxxx-xx
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HR: 0800h
AN: SH51A-1196
TI: Modeling of the heliospheric interface: multi-component model of the heliospheric plasma
AU: Malama, Y G
SH51A-1196 AF: Institute for Problems in Mechanics Russian Academy of Sciences, Prospekt Vernadskogo 101-1, Moscow, 119526 Russian Federation
AU: Malama, Y G
SH51A-1196 AF: Space Science Institute (IKI), Russian Academy of Sciences, Moscow, 117997 Russian Federation
AU: Malama, Y G
SH51A-1196 AF: Lomonosov Moscow State University, Department of Aeromechanics, School of Mechanics and Mathematics, Moscow, 119899 Russian Federation
AU: * Izmodenov, V V
EM: izmod@ipmnet.ru
AF: Institute for Problems in Mechanics Russian Academy of Sciences, Prospekt Vernadskogo 101-1, Moscow, 119526 Russian Federation
AU: * Izmodenov, V V
EM: izmod@ipmnet.ru
AF: Space Science Institute (IKI), Russian Academy of Sciences, Moscow, 117997 Russian Federation
AU: * Izmodenov, V V
EM: izmod@ipmnet.ru
AF: Lomonosov Moscow State University, Department of Aeromechanics, School of Mechanics and Mathematics, Moscow, 119899 Russian Federation
AU: Chalov, S V
SH51A-1196 AF: Institute for Problems in Mechanics Russian Academy of Sciences, Prospekt Vernadskogo 101-1, Moscow, 119526 Russian Federation
AU: Kallenbach, R
SH51A-1196 AF: International Space Science Institute, Switzerland, Bern, 3012 Switzerland
AB: We present a new model of the heliospheric interface - the region of the solar wind interaction with the local interstellar medium. This new model performs a multi-component treatment of charged particles in the heliosphere. All charged particles are divided into several co-moving sorts. The coldest sort, 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, electron impact ionization and photoionization are treated kinetically. The charged components are considered self-consistently with interstellar H atoms, which are described kinetically as well. To solve the kinetic equation for H atoms we use the Monte Carlo method with splitting of trajectories, which allows us 1) to reduce statistical uncertainties allowing correct interpretation of observational data, 2) to separate all H atoms in the heliosphere into several populations depending on the place of their birth and on the type of parent protons.
DE: 2124 Heliopause and solar wind termination
DE: 2126 Heliosphere/interstellar medium interactions
DE: 2144 Interstellar gas
DE: 2152 Pickup ions
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005


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