HR: 13:40h
AN: SH23A-01    [Abstracts]
TI: Propagation of the 12 May 1997 ICME in Evolving Solar Wind Structures
AU: * Odstrcil, D
EM: dusan.odstrcil@noaa.gov
AF: CU/CIRES and NOAA/SEC, 325 Broadway, Boulder, CO 80305 United States
AU: Pizzo, V J
EM: victor.pizzo@noaa.gov
AF: NOAA/SEC, 325 Broadway, Boulder, CO 80305 United States
AU: Riley, P
EM: pete@peteriley.org
AF: SAIC, 10260 Campus Point Drive, San Diego, CO 92121 United States
AU: Arge, C N
EM: nick.arge@hanscom.af.mil
AF: AFRL/VSBXS, 29 Randolph Road, Hanscom AFB, MA 01731 United States
AB: We simulate the 12 May 1997 interplanetary coronal mass ejection (ICME) event with a numerical 3-D magnetohydrodynamic (MHD) model, in which the background solar wind is determined from the SAIC and WSA coronal models, and the transient disturbance from the so-called cone model. We launch the same ICME-like, over-pressured plasma cloud into the background solar wind derived from various models including daily-updated coronal maps. We found that improved agreement with the observations is achieved when the maps are artificially modified to simulate the rapid displacement of one of the coronal hole boundaries after the CME eruption. We illustrate that multi-point temporal profiles of solar wind parameters and multi-perspective synthetic white-light images can be used to differentiate between various event scenarios that might be otherwise difficult to distinguish using single-point observations only.
DE: 7513 Coronal mass ejections
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2164 Solar wind plasma
DE: 3230 Numerical solutions
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting