HR: 08:50h
AN: SH51A-04    [PDF]
TI: An observation-based, hybrid 3D-MHD solar wind modeling system, H3DM
AU: * Fry, C D
EM: gfry@expi.com
AF: Exploration Physics International, Inc., Suite 37-105 6275 University Drive NW, Huntsville, AL 35806-1776 United States
AU: Wu, C
EM: ccwu@lepccwu.gsfc.nasa.gov
AF: Center for Space Plasmas and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL 35899 United States
AU: Wu, C
EM: ccwu@lepccwu.gsfc.nasa.gov
AF: Goddard Space Flight Center, National Aeronautics and Space Administration, Greenbelt, MD 20771 United States
AU: Detman, T R
EM: thomas.detman@noaa.gov
AF: Space Environment Center, National Oceanic and Atmospheric Administration, Boulder, CO 80305
AU: Smith, Z
EM: zdenka.smith@noaa.gov
AF: Space Environment Center, National Oceanic and Atmospheric Administration, Boulder, CO 80305
AU: Dryer, M
EM: murray.dryer@noaa.gov
AF: Center for Space Plasmas and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL 35899 United States
AU: Dryer, M
EM: murray.dryer@noaa.gov
AF: Space Environment Center, National Oceanic and Atmospheric Administration, Boulder, CO 80305
AU: Sun, W
EM: sun@jupiter.gi.alaska.edu
AF: Geophysical Institute, University of Alaska Fairbanks, Fairbanks, AK 99775 United States
AU: Deehr, C S
EM: cdeehr@gi.alaska.edu
AF: Geophysical Institute, University of Alaska Fairbanks, Fairbanks, AK 99775 United States
AU: Akasofu, S
EM: sakasofu@iarc.uaf.edu
AF: International Arctic Research Center, University of Alaska Fairbanks, Fairbanks, AK 99775 United States
AB: A major space weather challenge is to characterize and predict solar wind conditions, and in particular the evolution of the interplanetary magnetic field (IMF) near Earth. This requires modeling the non-uniform, ambient solar wind and tracking the propagation of interplanetary shocks and coronal mass ejections through the heliosphere. The mapping the IMF lines connecting the traveling shock region to the Earth is also required for predictions of solar energetic particles (SEP) and predictions based upon SEPs. Our group is developing an observation-driven, hybrid, kinematic/3D-MHD solar wind modeling system (H3DM) in order to simulate realistic solar wind conditions, including the time-dependent IMF vector (including Bz) direction and magnitude at Earth. This system couples two mature solar wind codes: the Hakamada-Akasofu-Fry (HAF) model and the Interplanetary Global Model, Vectorized (IGMV). Scientifically, this effort seeks to improve the understanding of the role various drivers of interplanetary disturbances play throughout the solar cycle. Operationally, we are working toward providing a capability to predict, shortly after the launch of large-scale structures at the Sun, their evolution and propagation to Earth. We will describe the H3DM modeling system and provide a project status report.
DE: 2134 Interplanetary magnetic fields
DE: 2139 Interplanetary shocks
DE: 2164 Solar wind plasma
DE: 2722 Forecasting
DE: 7513 Coronal mass ejections
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting