HR: 10:50h
AN: SH12B-03 [Abstracts]
TI: The Orientation of the Local Interstellar Magnetic Field and Induced Asymmetries of the Heliosphere: Neutrals-MHD model
AU: * Opher, M
EM: mopher@physics.gmu.edu
AF: George Mason University, 4400 University Drive, Fairfax, VA 22030, United States
AU: Stone, E C
EM: ecs@srl.caltech.edu
AF: California Institute of Technology, ECS: 220-47, Pasadena, CA 91125, United States
AU: Izmodenov, V
EM: izmod@ipmnet.ru
AF: Moscow State University, Department of Mechanics and Mathematics & Institute of
Mechanics, Moscow, 119899, Russian Federation
AU: Malama, Y
EM: malama@ipmnet.ru
AF: Institute for Problems in Mechanics Russian Academy of Sciences, Space Research
Insititute, Moscow, 119899, Russian Federation
AU: Alexashov, D
EM: izmod@ipmnet.ru
AF: Institute for Problems in Mechanics Russian Academy of Sciences, Space Research
Insititute, Moscow, 119899, Russian Federation
AU: Toth, G
EM: gtoth@umich.edu
AF: Center for Space Environment Modeling, 1416 Space Research Building, Ann Arbor, MI
48109-2143, United States
AU: Gombosi, T
EM: tamas@engin.umich.edu
AF: Center for Space Environment Modeling, 1416 Space Research Building, Ann Arbor, MI
48109-2143, United States
AB:
We present the results of a 3D Neutral-MHD model of the heliosphere. The neutrals are treated in a multi-fluid
approach coupled to the ionized component by charge exchange. Comparisons are made with previous studies
that showed that the local interstellar magnetic field introduces asymmetries in the heliosphere that are
consistent with Voyager 1 and 2 observations of radio emissions and energetic particle streaming (Opher et al.
Science 2007; Opher et al. ApJL 2006). We present, additionally, preliminary results of a 3D Kinetic-MHD model.
The main advantage of this model is a rigorous kinetic description of interstellar H atoms, especially at the Bow
Shock, Heliopause and Termination Shock interfaces. Differences of kinetic and multi-fluid approaches are
discussed. The new model should provide refined estimates of the strength and direction of the local interstellar
field and of the resulting distortions of the shape of the heliosphere.
DE: 2124 Heliopause and solar wind termination
DE: 2126 Heliosphere/interstellar medium interactions
DE: 2134 Interplanetary magnetic fields
DE: 2164 Solar wind plasma
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting