HR: 16:30h
AN: SH14A-03    [Abstracts]
TI: Three-dimensional global simulation of CME/ICME/Shock propagation from Sun to the heliosphere
AU: Wu, C
EM: wuc@cspar.uah.edu
AF: CSPAR/University of Alabama in Huntsville, 301 Sparkman Dr NW, TH S126, Huntsville, AL 35805 United States
AU: Fry, C
EM: gfry@expi.com
AF: Exploration Physics International, Inc., 6275 University Dr NW, Suite 37-105, Huntsville, AL 35806 United States
AU: Thompson, B J
EM: Barbara.J.Thompson@nasa.gov
AF: NASA/GSFC, NASA/GSFC, Greenbelt, MA 20771 United States
AU: * Wu, S
EM: wus@cspar.uah.edu
AF: CSPAR/University of Alabama in Huntsville, 301 Sparkman Dr NW, TH S126, Huntsville, AL 35805 United States
AU: Dryer, M
EM: murray.dryer@noaa.gov
AF: Exploration Physics International, Inc., 6275 University Dr NW, Suite 37-105, Huntsville, AL 35806 United States
AU: Dryer, M
EM: murray.dryer@noaa.gov
AF: NOAA/SEC, NOAA Space Environment Laboratory Center, R/E/SE, 325 Broadway, Boulder, CO NOAA Space United States
AU: Liou, K
EM: kan.liou@jhuapl.edu
AF: APL/Johns Hopkins University, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AB: This study performs simulations of the propagation of coronal mass ejections from the Sun to the Earth through a realistic 3D solar wind structure. The famous solar event of 12 May 1997, described observationally by Thompson et al. [1998, 1999] and theoretically by Wu et al. [2001], is used as motivation for this simulation. The newly developed code, HAF+3DMHD combines two simulation codes, Hakamada-Akasofu-Fry code (HAF) version 2 (HAFv.2) [Fry et al., 2001] and a fully three-dimensional, time-dependent MHD simulation code [Han et al, 1988]. The solar wind structure is simulated, using the HAF code, out to 0.08 AU from source surface maps derived from solar magnetograms. The HAF simulation is then used as input for the lower boundary of a 3D MHD code to calculate the evolution of solar wind plasma beyond 18 solar radii (0.08 AU). A dynamic disturbance is delivered to this non-uniform structure to model the evolution and interplanetary propagation of a coronal mass ejection (ICME, including its shock). We also integrate the changing line-of-sight heliospheric density to compare to data observed by the LASCO instrument on SOHO, and we compare the derived ICME and shock structure at 1 AU to WIND solar wind data for this 12 May 1997 event. This new code provides a tool to link the general cases of ICME at 1 AU to their solar sources, as well as to identify the possible origins of shock formation due to CMEs and CME/CIR interactions. In the case of complex or interacting ejecta, model interpretation is often required to accurately determine the solar sources of the ejecta observed at 1 AU. Because this newly developed model incorporates 3D MHD, its results can be extended to simulate coronal and heliospheric observations, including the ambient medium's non-uniformity provided by the HAFv.2 model, from the upcoming STEREO mission. Reference: Fry et al., JGR, 106, 20985-21001, 2001. Han et al., Comp. and Fluids, 16, 81-103, 1988. Thompson et al., GRL, 25, 2465-2468, 1998. Thompson et al., AP. J. Lett., 517, L151-L155, 1999. Wu et al., JGR, 106, 25089-25102, 2001.
DE: 2101 Coronal mass ejections (7513)
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2139 Interplanetary shocks
DE: 2169 Solar wind sources
DE: 7959 Models
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005