HR: 0800h
AN: SM51B-1303    [Abstracts]
TI: MHD Intermediate Wave Magnetosheath as Affected by Solar Wind MHD Disturbances and Magnetospheric Reconnection
AU: * Cable, S
EM: Sam.B.Cable@erdc.usace.army.mil
AF: Engineer Research and Development Center Major Shared Resource Center, 3909 Halls Ferry Rd., Vicksburg, MS 39180 United States
AU: Lin, Y
EM: ylin@physics.auburn.edu
AF: Dept. of Physics, Auburn University, Auburn University, Auburn, AL 36849 United States
AB: As is well-known, MHD (magnetohydrodynamics) simulations of the Earth's magnetosheath show that when the solar wind conditions are conducive to the formation of intermediate MHD shocks, the magnetosheath takes on a unique configuration, namely, convex outward with a very short standoff distance on the Sun-Earth line and extending relatively far away from the Earth on its flanks. Interactions between such a magnetosheath configuration and solar wind MHD waves that return the magnetosheath to a more ``conventional" configuration are simulated with a fully three-dimensional MHD code. Particular attention is paid to the generation, propagation, and reflection of MHD waves in the magnetosheath. The effect on the intermediate MHD magnetosheath configuration resulting from possible north-south asymmetries in magnetic reconnection rates between the solar wind and the Earth's magnetosphere will also be discussed.
DE: 2723 Magnetic reconnection (7526, 7835)
DE: 2728 Magnetosheath
DE: 2752 MHD waves and instabilities (2149, 6050, 7836)
DE: 2753 Numerical modeling
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Magnetospheric Physics [SM]
MN: Fall Meeting 2005