Friday 28 January 2011, by Alan Title (LMSAL, Palo Alto, CA, USA)
Thursday 3 February 2011 à 11h00 , Lieu : Salle de confĂ©rence du bât. 17
As the magnetic features on the solar are seen at higher and higher spatial and temporal resolution it becomes increasingly more difficult to recognize the polarity pairs in the flux emergence processes. Modern feature recognition processes identify more fragments than bipoles and even when “groups” are identified a significant fraction of the flux is neglected in the the analysis. Here I discuss a method that generates distributions on a pixel by pixel basis. It is discovered that the distributions have power laws indices of -2.2 to -3.5 in QS and -1 to -1.3 in plage. The measurements of the total and mean flux show there is have nearly perfect polarity balance in the inner network regions independent of radial position on the solar disk and independent of the flux imbalance of the surrounding network fields. If time allows some new results from the AIA mission will be described
