Abstract
We examine twisted magnetic flux ropes as the basic underlying magnetic field structure of CME precursors, and their loss of equilibrium as a mechanism for triggering CME onset. We present numerical simulations in spherical geometries of the evolution of the coronal magnetic field as a twisted magnetic flux rope is transported kinematically through the lower boundary into a pre-existing coronal potential arcade field. We find an initial quasistatic evolution during which a sequence of confined flux rope equilibria form with stored free magnetic energy, followed by a dynamic stage where the flux rope erupts. Finally, we also review simulation results on the dynamic process of how twisted magnetic flux ropes emerge from the high-β plasma of the interior through the photosphere into the solar corona.
| Original language | English |
|---|---|
| Pages (from-to) | 331-341 |
| Number of pages | 11 |
| Journal | European Space Agency, (Special Publication) ESA SP |
| Issue number | 596 |
| State | Published - 2005 |
| Event | International Scientific Conference on Chromospheric and Coronal Magnetic Fields - Katlenburg - Lindau, Germany Duration: Aug 30 2005 → Sep 2 2005 |
Keywords
- MHD
- Sun: corona
- Sun: magnetic fields