HR: 1340h
AN: SH13A-0302    [Abstracts]
TI: Towards a Realistic Model of Interacting CMEs in the Lower Heliosphere
AU: * Lugaz, N
EM: nlugaz@umich.edu
AF: CSEM - University of Michigan, 1424 Space Research Building 2455 Hayward Street, Ann Arbor, MI 48109-2143 United States
AU: Manchester, W
EM: chipm@umich.edu
AF: CSEM - University of Michigan, 1424 Space Research Building 2455 Hayward Street, Ann Arbor, MI 48109-2143 United States
AU: Roussev, I I
EM: iroussev@umich.edu
AF: CSEM - University of Michigan, 1424 Space Research Building 2455 Hayward Street, Ann Arbor, MI 48109-2143 United States
AU: Gombosi, T I
EM: tamas@umich.edu
AF: CSEM - University of Michigan, 1424 Space Research Building 2455 Hayward Street, Ann Arbor, MI 48109-2143 United States
AB: We first present a three-dimensional (3D) numerical ideal magnetohydrodynamics (MHD) model of interacting coronal mass ejections (CMEs). The simulation is based on an idealized 3D flux rope model of two CMEs propagating through a bimodal solar wind characteristic of solar minimum.
The different phases of the interaction are analyzed: propagation of the second CME into a perturbed heliosphere, shock-cloud interaction and shock-shock interaction. Properties of the complex ejecta at Earth, as well as evolutionary signatures of the interaction of the two CMEs are discussed. Transient phenomena, which could be observed by STEREO, are described.
We then focus on NOAA active region 9236, which produces a series of homologous CMEs/flares in November 24-26, 2000, associated with emerging magnetic flux. We discuss the difficulties of reproducing both the time-dependent coronal magnetic field structure and the solar wind's properties at 1 AU.
DE: 7513 Coronal mass ejections (2101)
DE: 7851 Shock waves (4455)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005