*Good set of data (relatively small b_z and b_t errors)
 
        *Balanced magnetic flux for the time series
 
        *Significant change in mean alpha before eruptive event
 
        *Linear fit alpha hardly varies compared to mean alpha
                                   
        *Significant changes in connectivity of field lines for the
          region of high activity and the moving feature

        *Build up of magnetic energy before the C-class flare

        *Free energy is very small
 
 
 
 

Next
-Find origins of the change in mean alpha
-Compare with coronal and chromospheric data
-Look at more active regions