HR: 12:00h
AN: SH12A-07    [Abstracts]
TI: An Integrated CME-SEP Numerical Investigation of the 1998 May 1-2 CME Events Part I: CME-Shock Models
AU: * Roussev, I I
EM: iroussev@umich.edu
AF: Department of AOSS, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109-2143 United States
AU: Sokolov, I V
EM: igorsok@umich.edu
AF: Department of AOSS, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109-2143 United States
AU: Tenishev, V
EM: vtenishe@umich.edu
AF: Department of AOSS, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109-2143 United States
AU: Liu, Y
EM: yliu@quake.stanford.edu
AF: W. W. Hansen Experimental Physics Lab, Stanford University, HEPL Annex, B210, Stanford, CA 94305-4085 United States
AU: Tylka, A J
EM: allan.tylka@nrl.navy.mil
AF: Space Science Division, Naval Research Laboratory, Code 7652, 4555 Overlook Avenue, SW, Washington, DC 20375-5352 United States
AU: Gombosi, T I
EM: tamas@umich.edu
AF: Department of AOSS, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109-2143 United States
AB: Improved understanding of solar eruptive phenomena requires developing more realistic coronal magnetic field models in which photospheric field measurements (e.g., MDI data) are used as a boundary condition for the magnetic field at the Sun, and the field is reconstructed in the corona using one of the standard extrapolation techniques (e.g., potential field source surface model). Apart from that, the plasma properties of the photosphere and solar corona are also needed to drive the models of solar eruptions. In this paper, we make a step forward in this direction, and we present data-driven numerical models of the CME events from 1998 May 1-2, which are two of the SHINE Campaign Events. We discuss the dynamics of the two eruptions and related shock waves in the low corona and interplanetary space. In our models, we adopt high-resolution magnetic data from MDI to set a realistic boundary condition for the radial magnetic field at the Sun. To initiate the CMEs, we slowly evolve the boundary conditions for the coupled tangential magnetic field and tangential plasma velocity at the solar surface in a way that resembles the observed dynamics of magnetic flux elements for the two events. The MHD model of each solar eruption is coupled with a SEP model. In this paper, we studied in detail the time-dependent changes in the shock strength and geometry over the course of the two eruptions, and we discuss the resulting SEP variability at the Earth. This investigation is funded by the NSF-SHINE Program.
DE: 7513 Coronal mass ejections (2101)
DE: 7514 Energetic particles (2114)
DE: 7526 Magnetic reconnection (2723, 7835)
DE: 7851 Shock waves (4455)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005