Solar Radiation Physical Modeling SRPM

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Solar Radiation Physical Modeling (SRPM)

• J. FontenlaJune 30, 2005b

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Mean Intensity
Emitted Spectra
Radiative Losses
and Net Radiative
Brackett
Atomic
Molecular
Continua
Continua
Radiative Transfer
Atomic Data
Molecular Data
Non-LTE
Molecular
Atomic
Lines
Lines
Populations Ionization
Balance
Atmospheric Parameters
Populations Ionization
Momentum Energy Balance
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Critical Next Steps

• Adjust photospheric models and abundances
• Low first-ionization-potential (FIP) contribute
  to ne and photospheric opacity
• High FIP are needed for upper layers
• Re-think lower chromosphere
• Account for radio data showing Tminlt4200 K
• Account for UV continua from SOHO-SUMER showing
  high Tmin
• Account for molecular lines (CN, CH, CO) showing
  low Tmin
• Re-think upper chromosphere with current
  abundances and observations
• Re-compute transition region with updated
  abundances, atomic data, diffusion and flows, and
  energy-balance
• MHD, full-NLTE, 3D simulations of chromospheric
  variations
• Prominence eruptions-CMEs

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Low Chromosphere Issues
Fe C abundance seem good
C I line
But computed CN lines are not good. Are
abundances incorrect? Or is the
model chromosphere incorrect?
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H Ionization and Ly Alpha Line
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V1.5 Ly? Computed Profiles

• Continuum too high due to Sulphur continuum
• Not enough contrast for faculae and plage
• Umbra profile has reversal unlike the observed

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Trace Species Ionization

• For each species and ionization stage

• Or split the abundance and ionization

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(No Transcript)
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Chromospheric Magnetic Heating Mechanism
Farley-Buneman Threshold Term
U, JHall
E,JPed
B
UthrCs(1?)
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Prominence-Eruption-CME

• 3-D non-LTE radiative transfer MHD modeling
• Instrumentation for observing Doppler spectra,
  spatial- and temporal-evolution