HR: 1340h
AN: SH14A-1690    [Abstracts]
TI: Three-dimensional magnetohydrodynamic modeling of the solar corona and solar wind for a highly-tilted solar dipole
AU: * Usmanov, A V
EM: arcadi.usmanov@nasa.gov
AF: NASA Goddard Space Flight Center, Heliophysics Science Division Code 673, Greenbelt, MD 20771, United States
AU: * Usmanov, A V
EM: arcadi.usmanov@nasa.gov
AF: University of Delaware, Bartol Research Institute, Newark, DE 19716, United States
AU: Goldstein, M L
EM: melvyn.l.goldstein@nasa.gov
AF: NASA Goddard Space Flight Center, Heliophysics Science Division Code 673, Greenbelt, MD 20771, United States
AB: A fully three-dimensional MHD model is used to simulate the global steady-state structure of the solar corona and solar wind for a solar magnetic dipole tilted by 60 and 90° to the solar rotation axis. The model accounts for the energy and momentum addition from Alfvén waves in the region between the base of the corona and Earth's orbit and for the effects of interstellar pickup protons in the outer heliosphere (1-100~AU). We present simulation results on the evolution of the heliospheric current sheet and the corotating interaction regions with heliocentric distance and on the effects of pickup protons in this evolution.
DE: 2102 Corotating streams
DE: 2149 MHD waves and turbulence (2752, 6050, 7836)
DE: 2152 Pickup ions
DE: 2164 Solar wind plasma
DE: 2169 Solar wind sources
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting