HR: 0830h
AN: P21F-03    [Abstracts]
TI: Solar Wind Conditions at Mars Predicted in Late 2003 and Early 2004
AU: * Fry, C D
EM: gfry@expi.com
AF: Exploration Physics International, Inc., Suite 37-105, 6275 University Drive NW, Huntsville, AL 35806 United States
AU: Dryer, M
EM: murray.dryer@noaa.gov
AF: Exploration Physics International, Inc., Suite 37-105, 6275 University Drive NW, Huntsville, AL 35806 United States
AU: Dryer, M
EM: murray.dryer@noaa.gov
AF: NOAA Space Environment Center, 325 Broadway, Boulder, CO 80305 United States
AU: Detman, T R
EM: thomas.r.detman@noaa.gov
AF: NOAA Space Environment Center, 325 Broadway, Boulder, CO 80305 United States
AU: Smith, Z
EM: zdenka.smith@noaa.gov
AF: NOAA Space Environment Center, 325 Broadway, Boulder, CO 80305 United States
AU: Wu, C
AF: CSPAR/UAH, Technology HAll, Room 101 University of Alabama in Huntsville, Huntsville, AL 35899 United States
AB: The solar wind plays a key role in the dynamics of the Martian upper atmosphere, ionosphere and radiation environment. The Hakamada-Akasofu-Fry (HAFv.2) solar wind model was used in a real-time prediction mode to forecast solar wind conditions and interplanetary shock arrival times at Mars in late 2003 and early 2004. The HAFv.2 model uses a modified kinematic approach to simulate solar wind speed, density, dynamic pressure and interplanetary magnetic field in the global heliosphere. The late 2003-early 2004 period included intervals of very disturbed solar wind observed at Earth. We compare simulations from the HAFv.2 model with data from the ACE L1 spacecraft near Earth, with observations in the close Martian environment, and with simulations by the Han-Wu-Dryer-Detman 3D-MHD solar wind model. The NASA Living With a Star Targeted Research and Technology Program is supporting this work.
DE: 1739 Solar/planetary relationships
DE: 2118 Energetic particles, solar
DE: 2164 Solar wind plasma
DE: 2722 Forecasting
SC: Planetary Sciences [P]
MN: 2005 Joint Assembly