WG4 Thursday 6-apr-06, joint session with WG2

Aurass

* 28 October 2003 (cf Klassen, Krucker et al. JGR 110, A09S04, 2005) via 
  signatures of relativistic protons, impulsive electrons, gradual electrons: 
  gradual electrons seem to be released late, 11:14-11:25)
* Schrijver-Derosa modeling of AR 10486 and 10493, finding N open field lines 
  in 493; large-scale loops and open field lines tend to avoid sites of 
  impulsive flare
* One hour of WIND-WAVES and Postdam observations. Focus on 11:12-11:20, the 
  GLE escape time range; locate "fiber burst" (intermediate drift) nest via 
  differentiation of spectrogram.
* What are these? Whistler waves interacting with trapped particles? A&A 2005 
  method involving a density model
* Early NRH source matches the flare loops (11:13-11:13); later one sees the 
  AR interconnecting loops
* Trottet 1994, metric source appearing during gamma-ray emission consistent 
  with this Fletcher, Pick, Hudson, Share (is there a connection with the 
  line narrowing)

Pick 

* Complementary observations from WIND, DAM, ARTEMIS, NRH show 11:15 as 
  a preferred time?
* EIT movie of fixed differences
Fletcher: link to different AR? Particle injection to the W, speculate about 
  shock waves interacting

Hudson (Schrijver)

* Lousy presentation of a difficult paper
Pick, Share, ...

Fletcher

* Introduction to thick-target beam problems. SHS (spectral correlations)
  and number (Holman estimates) leading to very large beam intensities
Vlahos - do we see the atmospheric response expected from the very intense
  heating?
Emslie - hearkening back 20 years, we have the double footpoints and 
  evaporation continuing. Now we have a worse picture
Hudson - foolish comment about moments of distribution function. Sensible
  comment about footpoint effective temperatures
Vlahos - what to do with enormous energy deposition? A fireball? Are the
  radiation hydro models good guides? (Emslie, Hudson, Fletcher...)

Grigis

* Evolution of electron distribution: Fokker-Planck with diffusion and
  convection. Assume U_T for wave energy density, get very hard spectrum
* Simple escape term 1/tau. Can keep constant particle number by ad hoc
  assumption - do this, and get SHS
* Pivot-point energy vs density negligible, somewhat on T in this framework
* A different model for escape: a potential barrier, eg to 40 keV, to get a
  20-keV pivot point 
Zharkova - where do the waves come from? Where does the return come from?
  It is just empirical.
Vlahos, Grigis, Zharkova, Fletcher, Warmuth. Preheating? Common need for hot
  Maxwellians?
Kontar - collision times? Few thousand gyrotimes

Pick

* Radio bursts and CMEs, 17 March 02, NRH + spectrometers
* MDI and RHESSI maps, 3 footpoints; NRH shows a series of IIIs moving NS
  (diagonally away) from the flare
* Continuum source displaced to W (up); CME almost due S shows good shock
  signature at side
Hudson - what about the bow wave? Puzzling, but when one does have a 
  signature it's usually at the flank, and seen by streamer kinks
* Potential-field extrapolation shows open field along the type III swarm,
  pointing directly in the direction of the CME axis
* Propose the type III beams to occur in the interface region to the open
  field, which increases in density compressionally; to 10x Newkirk for
  example  
Fletcher - see Khan spike-burst paper; Willson VLA observations