Splitting Flux Ropes: Modeling The Eruption Of Magnetic Structures On The Sun
Abstract
Coronal mass ejections (CMEs) and their associated space weather manifestations are routinely interpreted as possessing a helical magnetic flux rope structure. An ongoing controversy remains, however, as to whether a precursor flux rope exists as a coronal equilibrium state prior to eruption, or whether it is formed during eruption. This is an important question to resolve, since CME initiation models and space weather predictions depend upon a clear understanding of the configuration of pre-CME magnetic fields and their evolution during eruption. We will describe an alternative which lies between the two extremes of a totally erupting, pre-existing rope, and a rope that forms completely in situ during eruption, i.e., a precursor flux rope that splits in two and reconnects with surrounding fields during eruption. We consider the implications of such a "partially-expelled flux rope" model for a range of CME-related observations, including partially-erupting filaments, the evolution of post-flare loops and flare ribbon morphologies, and transient coronal holes.
- Publication:
-
American Astronomical Society Meeting Abstracts #210
- Pub Date:
- May 2007
- Bibcode:
- 2007AAS...210.5806G