Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.5804r&link_type=abstract
American Astronomical Society Meeting 210, #58.04; Bulletin of the American Astronomical Society, Vol. 39, p.168
Astronomy and Astrophysics
Astrophysics
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 former can explain the production of slow CME events (speeds less than 500km/s), whereas the latter, such as the breakout model, have the potential to describe the occurrence of fast events. The real Sun, however, demonstrates cases far more sophisticated 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 three-dimensional (3D) magnetohydrodynamic simulations, we investigated a possible physical scenario of the 2002 Apr 21 CME event. We used high-resolution MDI data to set realistic boundary condition for the magnetic field at the Sun. The loss of equilibrium and subsequent eruption are achieved by stretching and twisting the opposite polarities of a newly emerged magnetic dipole in the vicinity of AR9906 (source region). As the result of reconnection at 3D 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 neighborhood of AR9906. The CME dynamics proceeds in a manner different than that predicted by earlier models, yielding a fast event with properties similar to those of the observed one. This paper summarizes the simulated dynamics of the CME and their comparison with observations.
Lugaz Noé
Roussev Ilia I.
Sokolov Igor V.
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