Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1039..286r&link_type=abstract
PARTICLE ACCELERATION AND TRANSPORT IN THE HELIOSPHERE AND BEYOND: 7th Annual International Astrophysics Conference. AIP Confer
Astronomy and Astrophysics
Astrophysics
1
Magnetohydrodynamics And Plasmas, Planetary Bow Shocks, Interplanetary Shocks, Particle Acceleration, Solar Wind Plasma, Sources Of Solar Wind, Interplanetary Magnetic Fields
Scientific paper
The physical causes of coronal mass ejections (CMEs) have been debated by the solar community for over three decades now. The vast majority of proposed models agree that CMEs are the result of catastrophic loss of mechanical equilibrium or stability of the coronal magnetic field due to changes in the distribution of magnetic flux elements at the photosphere. These models usually involve idealized physical circumstances with either dipolar or quadrupolar underlying magnetic field geometries. The real Sun, however, demonstrates cases far more complex than those idealized configurations. Therefore, studying the actual magnetic field geometries involved during CMEs is crucial for understanding the dynamical time scales of the eruption, acceleration profiles, etc. By means of fully compressible 3-D magnetohydrodynamic simulations, we have investigated the CME events that took place on Apr 21 and Aug 24 of 2002. We have used high-resolution SoHO/MDI1 data to set realistic boundary condition for the magnetic field at the Sun. The loss of equilibrium and subsequent eruption have been achieved by stretching and twisting the opposite polarity feet of a newly emerged magnetic dipole in the vicinity of the source region of the CME. As the result of reconnection at 3-D null points, magnetic flux and helicity are transferred from the compact flux system containing the emerged dipole to the larger-scale flux systems in the neighboring active regions. The CME dynamics have been found to proceed in a manner different than that predicted by earlier models, yielding fast ejections with properties similar to those observed. This paper summarizes the simulated dynamics of the CMEs and associated shock waves, and their comparison with observations.
Lugaz Noé
Roussev Ilia I.
Sokolov Igor V.
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