file: OSLO1995.OUT = outline Oslo 1995 summer school
last: March 17 1995

================================= APPROACH =================================
Lecture notes
  \approx AFY course notes; AFY -> RTSA see RTSA.OUT
  but blackboard acts following NGSB
  
Transparencies
  IART XFIG plots
  NGSB data plots
  AFY2.1 equation \viewin cutouts

Time
  One 1/2 day = 2+1 lecture hours @ 45 min
  total: 11-12 lecture hours

Overview:
  half day 1  radiation quantities
              simple radiative transfer
  half day 2  LTE radiative transfer
              NLTE rate equations
  half day 3  NLTE radiative transfer
              spectral lines 
  half day 4  examples
                                             
================================= OUTLINE ==================================

Compilation of radiation quantities   2 hours; blackboard
-----------------------------------
  Intensity
    I?
    I_\nu               \nu+\Delta\nu  \lambda+\Delta\lambda
                        I_\nu = E/\Delta\nu
    more?               \Delta O, \Delta t
    \Delta \Omega       Novotny rays & beams
    I_\nu \equiv dE / dO dt d\nu d\Omega  
     
  Intensity on detector
    \delta \Omega
    irradiance
    surface flux
    interior flux
        
  I addition and extinction in a layer
    \Delta I?
      + j               what processes?  bb, bf, ff, Thomson, Rayleigh, .....
      - \alpha I        what processes?  just the reverse
       
  transport equation
    dI = j ds - alpha I ds
      
  optical pathlength/thickness/depth
    \exp{-\tau) decay
     
  source function
    S = j/alpha         ~ cow/horse
    nature
    2-level atoms
    excitation needs photons from wherever: J_\nu
    \varepsilon_\nu = photon destruction
    photon destruction
      collisional
      background continuum
      photon conversion
    photon creation
      idem 
    scattering versus thermal
       
Simple radiative transfer    1 hour  blackboard, IART
-------------------------
  transport equation
    dS/dtau = S - I
    integral solution
       
  homogeneous layer
    thin
    thick
    spectral lines
       
  stellar atmosphere
    Eddington Barbier
       
------------------------------------ 1/2 day -------------------------------
LTE radiative transfer   2 hours  transparencies 
----------------------
  TE conditions
    Planck
    Wien
    Rayleigh Jeans
    Maxwell
    Boltzmann
    Saha
    Saha-Boltzmann
    
  LTE formation of continua and lines from stellar atmospheres
    solar continua
    H_min
    solar continuum limb darkening
    solar line profiles
    solar line limb darkening
      
NLTE rate equations   1 hour  transparencies
-------------------
  bound-bound processes
    Einstein coefficients
    line j, alpha, S
    departure coefficients
      
  continuum processes
    bf, ff
    Thomson, Rayleigh scattering

  SE rate equations
  
  net rates
    expressed in b's
    
------------------------------------ 1/2 day ------------------------------

Thick: NLTE radiative transfer  2 hours  transparencies
------------------------------
  Intensity moments
  Lambda operator
  Diffusion approximation
  Eddington approximation
  \sqrt \varepsilon law 
  Examples of J-B divergences
    continua VALIII
    ionization FeI
    line haze

Spectral lines  1 hour  transparencies
--------------
  Line broadening
  Redistribution
  Velocity gradients

---------------------------------- 1/2 day --------------------------------

Examples  2 hours
--------
  Thin: coronal conditions
    rate equations
    dieelectronic recombination
    ionization equilibria
        
  Thick: solar NaD in detail

  Thick + atmosphere: Mihalas + Auer hot star