HR: 0800h
AN: SH51A-1199    [Abstracts]
TI: Implications for Voyager 1 and Voyager 2 Observations From 3D Modeling and Analysis of the Interplanetary Propagation of Solar-Induced Shock Waves
AU: * Intriligator, D S
EM: devriei@aol.com
AF: Carmel Research Center, P.O. Box 1732, Santa Monica, CA 90406-1732 United States
AU: Sun, W
EM: sun@jupiter.gi.alaska.edu
AF: Geophysical Institute, University of Alaska, Fairbanks, AK 99755 United States
AU: Detman, T R
EM: Thomas.R.Detman@noaa.gov
AF: NOAA/SEC, 325 Broadway, Boulder, CO 80305 United States
AU: Detman, T R
EM: Thomas.R.Detman@noaa.gov
AF: Exploration Physics International, 6275 University Drive #37-105, Huntsville, AL 35806-1776 United States
AU: Fry, C D
EM: gfry@expi.com
AF: Exploration Physics International, 6275 University Drive #37-105, Huntsville, AL 35806-1776 United States
AU: Dryer, M
EM: murray.dryer@noaa.gov
AF: NOAA/SEC, 325 Broadway, Boulder, CO 80305 United States
AU: Dryer, M
EM: murray.dryer@noaa.gov
AF: Exploration Physics International, 6275 University Drive #37-105, Huntsville, AL 35806-1776 United States
AU: Deehr, C
EM: cdeehr@gi.alaska.edu
AF: Geophysical Institute, University of Alaska, Fairbanks, AK 99755 United States
AU: Intriligator, J
EM: j.intriligator@bangor.ac.uk
AF: Carmel Research Center, P.O. Box 1732, Santa Monica, CA 90406-1732 United States
AU: Intriligator, J
EM: j.intriligator@bangor.ac.uk
AF: Centre for Neuroscience, University of Wales, Bangor, Wal LL572AS United Kingdom
AB: We use the three dimensional HAFv2 (Hakamada-Akasofu-Fry version 2) kinematic solar wind model to study the interplanetary propagation of solar-induced shock waves from the Sun to 96 AU and over a wide range of heliolongitudes and heliolatitudes. We compare the HAFv2 model predictions at ACE (1 AU), Ulysses (5.4 AU), Voyager 2 (76 AU), and Voyager 1 (96 AU) to available data. In addition, we use the three dimensional MHD HHMS (Hybrid Heliospheric Modeling System) to further study the more detailed evolution of interplanetary magnetic field and plasma parameters to 10 AU. Statistical analyses between the data and the results from the 3D models for distances to 10 AU show high correlation coefficients. Our analyses further indicate that all of the spacecraft are observing the effects of solar events.
DE: 2114 Energetic particles (7514)
DE: 2124 Heliopause and solar wind termination
DE: 2134 Interplanetary magnetic fields
DE: 2139 Interplanetary shocks
DE: 2164 Solar wind plasma
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005