NSF Site Visit Madison, May 1-2, 2006 Magnetic Helicity Conservation and Transport R. Kulsrud and H. Ji for participants of the Center for Magnetic Self-organization.
How much helicity is needed to drive large-scale dynamos?
1. Background2. Flux variation3. Polarity reversal4. Electron evolution5. Conclusions The role of coronal mass ejections in the solar cycle evolution of.
