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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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"SH51A-1198"
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HR: 0800h
AN: SH51A-1198
TI: Effects of the interstellar magnetic field on the shape of the inner heliosheah and on the penetration of interstellar neutrals in the heliosphere
AU: Alexashov, D
EM:
AF: Institute for Problems in Mechanics Russian Academy of Sciences, Prospekt Vernadskogo 101-1, Moscow, 117526 Russian Federation
AU: Alexashov, D
EM:
AF: Space Research Institute (IKI) Russian Academy of Sciences, Russian Academy of Sciences, Moscow, 117997 Russian Federation
AU: * Izmodenov, V
EM: izmod@ipmnet.ru
AF: Institute for Problems in Mechanics Russian Academy of Sciences, Prospekt Vernadskogo 101-1, Moscow, 117526 Russian Federation
AU: * Izmodenov, V
EM: izmod@ipmnet.ru
AF: Space Research Institute (IKI) Russian Academy of Sciences, Russian Academy of Sciences, Moscow, 117997 Russian Federation
AU: * Izmodenov, V
EM: izmod@ipmnet.ru
AF: Moscow State University, Department of Aeromechanics and Gas Dynamics, School of Mechanics and Mathematics, Moscow, 119899 Russian Federation
AB: Recently Lallement et al. (2005, Science, 307, 1447) reported that the direction of the flow of interstellar neutral hydrogen in the heliosphere is deflected by ~4° from the direction of the pristine local interstellar gas flow. The most probable physical phenomenon responsible for such a deviation is the interstellar magnetic field inclined to the direction of the interstellar gas flow. In this case the flow of the interstellar charged component is asymmetric and distorted in the region of the solar wind interaction with the local interstellar medium, which is called the heliospheric interface. The interstellar H atoms pass through the heliospheric interface and interact with the plasma component by charge exchange. Some imprints of the asymmetry of the heliospheric plasma interface should be seen in the distribution of the interstellar H atom component. In this letter we explore this scenario quantitatively and demonstrate that our new self-consistent 3D kinetic-MHD model of the solar wind interaction with the magnetized interstellar plasma is able to produce the measured deviation in the case of a rather strong interstellar magnetic field of ~2.5 μG inclined by ~45° to the direction of interstellar flow. Shapes and locations of the TS and the HP are discussed.
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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