WG4 Friday morning session

Sui

* Oops - so interesting I forgot to start taking notes.
* "Preheating" vs early spike RHESSI events
Hudson: "preheating" is tendentious in view of SXT tendency for flare loops
  to start from empty regions
* 3-6 keV impulsive profile in extreme event
* Fe feature at 6.7 keV with no requirement for a thermal continuum (!)
Fletcher, Dennis, Hudson
* Modeling of evaporation: loop density, SHS, cutoff energy variation
Ji
Fletcher, Warmuth
Warmuth - can we really go to 3 keV? Dennis - in A0 even, still must be
  careful. 5 1/3 keV lower limit usual choice.
Fletcher - K escape? Explanation of K escape by BRD

Hudson

* Can't talk and type at the same time - see the published paper please,
  Solar Physics March 2006
Much discussion, including FLetcher material on energetics

Dennis

* Flare/CME energies: GOES L_SXR, L_hot, CME kinetic energy KE_CME from
  Gopalswamy
* Analysis includes 64 CMEs and 138 GOES flares from the October 2003 interval;
  Flare ID by CME height-vs-time trajectory
* Flare/CME start times => flares first +-
* Flare/CME kinetic energies by component: pretty good correlation between
  KE_CME and L_hot over 4 decades, at about 1/10
* Refined correlation plot incorporating SORCE/TIM information
* SORCE observations of 28-Oct illustrating the impulsive-phase component 
Discussion of precision of SORCE observations - precision of lower limit good
  to a factor 2, perhaps upper limit larger still
* Bottom-line result: L_tot ~ KE_CME ~ 10L_hot ~ 100L_SXR