HR: 09:30h
AN: SH41B-07 INVITED     [Abstracts]
TI: Interaction of the solar wind and the interstellar medium: global structure
AU: * Zank, G P
EM: zank@ucr.edu
AF: IGPP, University of California, Riverside, CA 92521 United States
AB: The global structure of the heliosphere is determined by a combination of the interstellar plasma pressure, the movement of the Sun through the ISM, the interstellar magnetic field, and the interstellar neutrals, and of course, the supersonic solar wind itself. It can be affected by variability in the solar wind (solar cycle dependent) and by variability in the interstellar environment. The past 5 years has seen the development of sophisticated 2D steady-state models of the heliosphere that incorporate much of the basic physics thought to determine structure. More recent developments have begun to focus on the inclusion of time dependence, fully 3D structure (which implies the inclusion of the interplanetary and interstellar magnetic fields), and more sophisticated physical processes such as galactic and anomalous cosmic rays, turbulence excited by pickup ions, and so forth. We will review the modeling efforts of the past 5 years, relate this to observational tests, both current and proposed, and discuss briefly new directions and trends.
DE: 2124 Heliopause and solar wind termination
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting