HR: 0800h
AN: SH51A-06    [Abstracts]
TI: Comparing various multi-component global heliosphere models
AU: * Mueller, H R
EM: hans.mueller@dartmouth.edu
AF: Dartmouth College, Dept. of Physics and Astronomy, Hanover, NH 03755, United States
AU: * Mueller, H R
EM: hans.mueller@dartmouth.edu
AF: IGPP-UCR, 900 University Ave., Riverside, CA 92521, United States
AU: Florinski, V
EM: vflorin@ucr.edu
AF: IGPP-UCR, 900 University Ave., Riverside, CA 92521, United States
AU: Heerikhuisen, J
EM: jacobh@ucr.edu
AF: IGPP-UCR, 900 University Ave., Riverside, CA 92521, United States
AU: Izmodenov, V
EM: izmod@ipmnet.ru
AF: Lomonosow Moscow State University, Department of Mechanics and Mathematics and Institute of Mechanics, Moscow, 119899, Russian Federation
AU: Izmodenov, V
EM: izmod@ipmnet.ru
AF: Institute for Problems in Mechanics, Russian Academy of Sciences, Moscow, 119526, Russian Federation
AU: Scherer, K
EM: kls@tp4.rub.de
AF: Ruhr-University Bochum, Institute for Theoretische Physik IV: Weltraum- und Astrophysik, Bochum, 44780, Germany
AU: Alexashov, D
EM: izmod@ipmnet.ru
AF: Institute for Problems in Mechanics, Russian Academy of Sciences, Moscow, 119526, Russian Federation
AU: Fahr, H J
EM: fahr@uni-bonn.de
AF: Argelander Institute for Astronomy, Dept. of Astrophysics University of Bonn Auf dem Huegel 71, Bonn, 53121, Germany
AB: Modeling of the global heliosphere seeks to investigate the interaction of the solar wind with the partially ionized local interstellar medium. Models that treat neutral hydrogen self-consistently and in great detail together with the plasma, but neglect magnetic fields, constitute a sub-category within global heliospheric models. There are several different modeling strategies used in the literature, and this contribution seeks to point out differences and commonalities in the modeling results from different strategies. Plasma-only models, and fully self- consistent models from four research groups, for which the neutral species is modeled with either one, three, or four fluids or kinetically, are run with the same boundary parameters and equations. They are compared to each other with respect to the locations of key heliospheric boundary locations, and with respect to the neutral hydrogen content throughout the heliosphere. In many respects, the models basically agree. In particular, the locations of the termination shock agree to within 7% in the nose direction and to within 14% in the downwind direction. The nose locations of the heliopause agree to within 5%. The filtration of neutral hydrogen from the interstellar medium into the inner heliosphere, however, is model dependent, and possible physical reasons for this are discussed.
DE: 2124 Heliopause and solar wind termination
DE: 2126 Heliosphere/interstellar medium interactions
DE: 2144 Interstellar gas
DE: 7837 Neutral particles (2151)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Joint Assembly