HR: 0800h
AN: SH32A-0783 [Abstracts]
TI: Numerical Simulation of a Coronal Mass Ejection in the Lower Corona: Comparison of Two Initiation Models
AU: * Loesch, C
EM: cristiane@plasma.inpe.br
AF: George Mason University, 4400 University Drive
MSN 3F3, Fairfax, VA 22030-4444, United States
AU: * Loesch, C
EM: cristiane@plasma.inpe.br
AF: Instituto Nacional de Pesquisas Espaciais, Av. dos Astronautas 1758
Laboratório Associado de Plasma, São José dos Campos, SP 12227-010, Brazil
AU: Opher, M
EM: mopher@physics.gmu.edu
AF: George Mason University, 4400 University Drive
MSN 3F3, Fairfax, VA 22030-4444, United States
AU: Liu, Y
EM: yliuc@gmu.edu
AF: George Mason University, 4400 University Drive
MSN 3F3, Fairfax, VA 22030-4444, United States
AU: Manchester IV, W B
EM: chipm@umich.edu
AF: CSEM University of Michigan, Space Research Building 2455 Hayward Street, Ann Arbor, MI
48109, United States
AU: Gombosi, T I
EM: tamas@umich.edu
AF: CSEM University of Michigan, Space Research Building 1517, Ann Arbor, MI 48109, United
States
AU: Alves, M V
EM: virginia@plasma.inpe.br
AF: Instituto Nacional de Pesquisas Espaciais, Av. dos Astronautas 1758
Laboratório Associado de Plasma, São José dos Campos, SP 12227-010, Brazil
AB:
Coronal mass ejections (CME), eruptions of plasma and embedded magnetic field from the Sun's corona into
interplanetary space, are the most energetic events on the Sun. The exact processes involved in the release of
CMEs are not known. In order to understand them and how they affect the environment around Earth we need to
comprehend their eruption, development and propagation through the interplanetary space. In this work, we
present a simulation of a CME event occurred during the solar minimum. This simulation was performed using
the Space Weather Modeling Framework (SWMF). Within this model, after generating a global steady state of the
solar corona, for CR1922, we drive a CME to erupt using two different initiation models presented in the literature;
Gibson and Low (1998) and Titov and Démoulin (1999). The ejections, that were followed up to distances of 10
R\sun, reached maximum speeds of 800-1000 km s-1. We discuss these two CME initiation models
establishing a comparative analysis of their characteristics and how the initiation process changes the evolution
of a simulated CME.
DE: 2101 Coronal mass ejections (7513)
DE: 7900 SPACE WEATHER
DE: 7959 Models
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting