file: schedule.txt = "Solar Spectrum Formation" @ NAOJ May 2016
init: Apr  6 2016  Shin Toriumi
last: May 24 2016  Rob Rutten  Mitaka
note: evolved from plan to log
      usual: # comment, @ todo 
     

     NAOJ Lecture Course "Solar Spectrum Formation"


------------------ SCHEDULE --------------------------

Goal: become optically thick in preparation of Solar-C

Content
  line and continuum particle-photon processes
  radiative transfer
  thin cloud > LTE > NLTE > PRD > non-E > Solar-C lines
  [no polarimetry]

Dates: 2016 May 16-20

Morning
  09:00-09:50  lecture
  10:00-10:50  lecture
  11:00-11:50  lecture 

Lunch

Afternoon 
  13:00:13:45  lecture
  14:00-17:00  participant 5-min presentations (Mon & Tue)
               practicals 


------------------ DAY BY DAY LOG ----------------------------

Monday May 16 - Cosmos Kaikan
  Birth of astrophysics
    DIY spectral classification (practical SSA1)
    empirical HRD
    Saha-Boltzmann
      Cecilia Payne
      solar CaIIK versus Halpha 
      Saha-Boltzmann for chromospheric lines
  exercise contents
  Basic solar spectrum formation (lecture file SSI)
    continuum
      observed intensity > depth of viewing > Hmin extinction
    lines
      bb processes
      bb process pairs: collisional or scattering addition or reduction
      photospheric line = map extinction and source function via depth

  5-minute presentations (first batch)
    @ photograph each  

  Example: coronal radiation
    white-light corona = Thomson scattering with Fraunhofer line erasure
    forbidden optical lines = very high ionization stages
    EUV coronal line formation = coronal equilibrium = thermal photons
    EUV dark = bound-free scattering HI, HeI, HeII edges out of passband

  Practical
    SSA2 = Saha Boltzmann ("Cecilia Payne")


Tuesday May 17 - Cosmos Kaikan
  Basic radiative transfer 
    repeat bb processes and pairs > extinction and emissivity (white board)
    quantities
    intensity conservation including exam (in break)
    source function
    (S,alpha) combination more orthogonal than (j,alpha)
    transport equation
    constant-S cloud lines: thick, thin, core saturation
    plane-parallel RT 
    Eddington-Barbier, with cartoons
  LTE plane-parallel spectrum formation
    continua
       demo: HI and H-min in solar atmosphere
       @ add my Gray plots, Vitense confusograms (idl/edulib)
    lines
    limb darkening
    line broadening
    4-panel Eddington-Barbier line and edge formation cartoons
   
  Examples: solar spectrum per LTE
    ultraviolet line flip
    VAL3C temperature
    @ add Kurucz stellar LTE spectra

  5-minute presentations (rest)

  Practicals: SSA, SSB

Wednesday May 18 - Student seminar room 
  Avrett solar spectrum cartoon
  Intermezzo: MgI 12-micron emission lines
  Radiative transfer with scattering
    J
    lambda operator
    2-level source function
    sqrt(eps) law, thermalization depth
    Avrett 2-level results
    SE equations

  mugshot collection # better at start (first break) @ process first evening

  Practicals: SSA, SSB

Thursday May 19 - Cosmos Kaikan
  Scattering summary 
  More line-formation complexity
    @ RE: derivation - grey - non-grey - scattering
    partial redistribution
      @ cartoon profile bad, improve
      @ simplified Hummer R functions 
      @ cartoon atom-frame vs observer-frame Doppler
    multi-level detours 
      # should have done planetary nebulae here
    lambda iteration

  Examples
    NLTE 1D continuum formation 
      VALIIIC continua
      VALIIIC radiation energy budget
  
  Practical: SSB
 
Friday May 20 - Cosmos Kaikan
  Summary
    equation summary 
    NLTE summary

  Examples  
    chromospheric line formation
      1D-SE standard model: NaID, MgIb, CaII8542, CaIIK, MgIIk, Halpha
      thermalization Ly-alpha S^l gives LTE Halpha extinction
      clapotisphere (1D HD Radyn) 
        Carlsson line formation breakdown plots
        standard models describe shocks, not mean temperature
      non-E hydrogen (2D MHD Stagger)
      Halpha recipe: LTE extinction in hot and dense onsets, maintain value
    fibrils as contrails
      Halpha versus CaII8542
      Halpha versus Lyalpha
      expectation for ALMA

  Course homework = Auer & Mihalas star (last problem in RTSA notes)

  Course moral
    target 
      "where is my line formed?" > course examination 
    solar atmosphere scene
    on beauty

  Practical: SSB

------------------ SKIPPED ----------------------------

theory
    polarization
    radiative equilibrium, line blanketing
    frequency redistribution functions
    angle redistribution
    Halpha S^l not Thomas "photoelectric control" but 2-level scattering

examples
    planetary nebulae Halpha and nebulium lines (drastic photon conversion)
    NLTE masking (ultraviolet overionization depletes opacity optical lines)
    Milne-Eddington and inversions (simplistic best-fit modeling)
    magnetic bright points (holes in cont, FeI, G-band, Halpha, ultraviolet)
    faculae versus irradiance modeling (MnI lines are the only reliable)
    reversed granulation (line flank steepness makes NaID champion)
    NaID shocks in fluxtubes (NaID Dopplergrams are sharpest magnetograms)
    limb emission lines (interlocking, ultraviolet pumping, PRD)
    Ellerman bomb visibilities (LTE extinction in hot onsets)
    atomic blends in IRIS profiles (slanted LOS through irradiated clap)

exercises
    questions in IART notes; problems at end of RTSA notes; SSC practical


------------------ PARTICIPANTS -----------------------------

  Yusuke Kawabata, ISAS/JAXA
  Takayoshi Oba, ISAS/JAXA
  Takahiro Hasegawa, ISAS/JAXA
  Takafumi Doi, ISAS/JAXA
  Yikang Wang, Univ of Tokyo
  Shunya Kono, Univ of Tokyo
  Haruhisa Iijima, Nagoya Univ
  Yuwei Huang, Kyoto Univ
  Akiko Tei, Kyoto Univ
  Yuta Notsu, Kyoto Univ
  Kousuke Namekata, Kyoto Univ
  Denis Cabezas, Kyoto Univ
  Takahito Sakaue, Kyoto Univ
  Nagaaki Kambara, NAOJ
  Masaki Yoshida, NAOJ
  Yoshiki Hatta,  NAOJ
  Shin Toriumi, NAOJ
  Kyoung-Sun Lee, NAOJ
  Anand Joshi, NAOJ
  Ryoko Ishikawa, NAOJ
  Masahito Kubo, NAOJ
  Joten Okamoto, NAOJ