1. MSU Team: R. C. Canfield, D. W. Longcope, P. C. H. Martens, S. Régnier Evolution on the photosphere: magnetic and velocity fields 3D coronal magnetic fields from IVM vector magnetograms Boundary conditions for driving magnetohydrodynamic codes Solar MURI project Solar Eruptions and their Interplanetary Consequences: Observations and Modeling from the Photosphere to the Corona

2. Evolution on the photosphere: magnetic and velocity fields Long term evolution MDI line-of-sight magnetograms (5 days, -30 o -+30 o ) - Analysis of the photospheric magnetic field for AR8210 - Analysis of a time series of IVM/MSO vector magnetograms Short term evolution IVM vector magnetograms (~ 4 h 30 min)

3. Evolution on the photosphere: magnetic and velocity fields - New method to determine the velocity field (Longcope et al., 2002); - Determination of the magnetic energy rate and the magnetic helicity rate from IVM vector magnetograms and velocity fields (Δt = 15 min); - Correlation between the Hα flaring regions and the injection of magnetic helicity; - Future works: calculations for a Δt of ~3 min, links between injection rates and 3D magnetic fields.

4. 3D coronal magnetic fields from IVM vector magnetograms Non-constant-α force-free equilibrium state describing the coronal magnetic field of AR8210 (Régnier, Amari & Canfield, 2002); Complex topology of AR8210 (separatrix surfaces) Free magnetic energy: 1.7% of the magnetic energy

5. Boundary conditions for driving magnetohydrodynamic codes Photospheric vector magnetograms Photospheric velocity fields 3D coronal magnetic field as initial equilibrium state