file: oslo2007.pln
last: Jun 18 2007 
init: Jun 14 2007 = copy oslo2003.pln
todo: 
  answers problems in Oslo dir
  pdf in Oslo dir
  viewgraph VALIIIC for reference overhead
  viewgraph outline
  print participant-mats.txt voor in broekzak
  koop summer map (waar?)

schedule
========
  hour 1  08:30-09:15
  break                09:15-09:30
  hour 2  09:30-10:15 
  break                10:15-10:30
  hour 3  10:30-11:15 
  break                11:15-11:30
  problem 11:30-12:00


Tuesday 
=======

  hr 1 = examples without RT  # vw
  ----------------------------------
  intro
+   vw  outline
+   vw  Muench painting 

  EUV corona = local thermal photons
+   vw  TRACE something tangled = much more beautiful & understandable
        coronal EUV radiation
        5 processes bb, bf, ff
        coronal    and bf process combinations
        coronal equilibria      = f(T)   bf = f(T,N_e)
+   vw  Jordan iron ionization curves
        dielectronic recombination
        thermal radiation: S=B?  LTE?  
 
  white-light corona = non-local scattered photons
+   vw white light corona (Wielinga)
+   vw white light \approx 6000 Planck
+   vw Kitt Peak solar spectrum 
       Fraunhoferspectrum in this room
       Rayleigh scattering earth atmosphere preserves frequency
       K corona = no lines 
       Grotrian: high-speed electron scattering 
+   vw van der Hulst graph 

  planetary nebulae = non-local converted photons
+   vw HST M57 = ring nebula in Lyra
+   vw spectrum
+   vw Zanstra hydrogen = doubly non-local (location, wav)
+   vw Bowen nebulium pumping = triply non-local (location, wav, species) 


@ hr 2 = basic stellar-atmosphere RT # pdf
  ----------------------------------
         repeat corona
         basic quantities
         homogeneous layer
         thick transfer
      
@ hr 3 = LTE solar radiation escape # pdf
-----------------------------------
   Planck
   H-minus in LTE
   Boltzmann-Saha
   Schadeenium in LTE
   LTE lines
   simple absorption line
   simple emission line
   solar ultraviolet spectrum
   VALIIIC model
   solar spectrum formation
   CaII H versus Halpha  

+ hr 4 =  problem 1 
-------------------

Wednesday  ### not necessarily with these breaks, better start on 3 in hour 2
=========

@ hr 1 = radiative transfer math
--------------------------------
         transport, moment equations
         operators
         Kourganoff plots
         Krijger plots

+ hr 2 = 2-level scattering # vw = Chapt 4 equations, Chapt 4 plots
---------------------------
         Zwaan illustration Eddington approximation
         square root epsilon law
         thermalization 
         Avrett plots

@ hr 3 = NLTE solar radiation escape # pdf
----------------------
      bb processes
      bb rates
      bb equilibria
      solar radiation processes
      realistic absorption line
      VAL3C continuum formation
      radiative cooling
      VAL3C radiation budget
      Na D1
      Na D1 blends 

+ hr 4 =  problem 7 
-------------------


Participants
============
Ad'en, Daniel   
Antolin, Patrick
Belluzzi, Luca  
Cseki, Attila   
Danilovic, Sanja  
Fischer, Catherine
Gonzalez, Nazaret Bello 
Gunar, Stanislav        
Guver, Funda Bostanci   
Hayek, Wolfgang         
Henriques, Vasco        
Hillberg, Tomas         
Laursen, Peter          
Leenaarts, Jorrit       
Matthews, Owen          
Meling, Martin          
Murakozy, Judit         
Naram, Gautam           
Olshevsky, Vyacheslav   
Pereira, Tiago          
Rodriguez Gasen, Rosa   
Rodriguez, Jaime de la Cruz   
Shapiro, Alexander      
Felipe Garcia, Tobias   
van Marle, Allard-Jan   
Vecchio, Antonio        
Vitas, Nikola           
Vornanen, Tommi         
Xu, Zhi                 
Yelles Chaouche, Lotfi  
Zacharias, Pia          
Zverina, Pavel          

Oslo
----
Juan Martinez Sykora  
Silje Bjolseth   
Oystein Langangen
Leandro Gomez di Jesus