HR: 1340h
AN: SH43A-1082    [Abstracts]
TI: Possible Effects at Voyager 1 and Voyager 2 of Solar Events
AU: * Intriligator, D S
EM: devriei@aol.com
AF: Carmel Research Center, P.O. Box 1732, Santa Monica, CA 90406 United States
AU: Sun, W
EM: sun@jupiter.gi.alaska.edu
AF: Geophysical Institute, University of Alaska, Fairbanks, AK 99775 United States
AU: Fry, C D
EM: gfry@expi.com
AF: Exploration Physics International, Inc., University Drive, NW, Huntsville, AL 35806 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: Dryer, M
EM: murray.dreyer@noaa.gov
AF: Exploration Physics International, Inc., University Drive, NW, Huntsville, AL 35806 United States
AU: Dryer, M
EM: murray.dreyer@noaa.gov
AF: NOAA/Space Environment Center, 325 Broadway, Boulder, CO 80305 United States
AU: Deehr, C
EM: cdeehr@gi.alaska.edu
AF: Geophysical Institute, University of Alaska, Fairbanks, AK 99775 United States
AU: Intriligator, J
EM: j.intriligator@bangor.ac.uk
AF: Carmel Research Center, P.O. Box 1732, Santa Monica, CA 90406 United States
AU: Intriligator, J
EM: j.intriligator@bangor.ac.uk
AF: University of Wales, Brigantia Building, Bangor, Wal LL572AS United Kingdom
AB: Recent Voyager observations are analyzed in the context of the propagation of solar events to the outer heliosphere. The three-dimensional HAFv2 model results show that solar events can asymmetrically propagate to the outer heliosphere. Both longitudinal and latitudinal asymmetries may be important. We compare the preliminary HAFv2 model results with in-situ solar wind plasma, interplanetary magnetic field, and energetic particle observations from Voyager. We also compare the HAFv2 predictions with those from other models.
DE: 2104 Cosmic rays
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2114 Energetic particles, heliospheric (7514)
DE: 2124 Heliopause and solar wind termination
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting