Quantitative modeling of magnetic reconnection creating a twisted flux rope
Abstract
Coronal mass ejections (CMEs) are one of the key elements coupling solar activity throughout the heliosphere. A two-dimensional model, called CSHKP has been used to explain the observed sequence of events in a typical CME. They are launched from the solar corona above reversals in photospheric magnetic polarity. Chromospheric emission during the accompanying two-ribbon flare provides evidence of magnetic reconnection. Magnetic clouds, structures observed in situ, are believed to be twisted magnetic flux ropes launched into space by the CME. Here I demonstrate a three-dimensional generalization of the CSHKP model. This model provides a quantitative picture of how reconnection in a two-ribbon flare can produce a twisted flux rope from an arcade of slightly sheared coronal field lines. It quantifies relationships between the initial shear, the amount of flux reconnected and the total axial flux in the twisted rope. The model predicts reconnection occurring in a sequence which progresses upward even if the reconnection sites themselves do not move. This work was supported by NSF through grant ATM-0416340.
- Publication:
-
AGU Spring Meeting Abstracts
- Pub Date:
- May 2008
- Bibcode:
- 2008AGUSMSH31C..02L
- Keywords:
-
- 7513 Coronal mass ejections (2101);
- 7526 Magnetic reconnection (2723;
- 7835)