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Solar Radiation Physical Modeling (SRPM) PowerPoint Presentation

Solar Radiation Physical Modeling (SRPM)

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### Solar Radiation Physical Modeling (SRPM)

J. FontenlaJune 30, 2005b

Emitted Spectra

Radiative Losses

and Net Radiative

Brackett

Atomic

Molecular

Continua

Continua

Atomic

Data

Radiative Transfer

Molecular

Data

Non-LTE

Molecular

Atomic

Lines

Lines

Populations &

Ionization

Balance

Populations &

Ionization

Atmospheric

Parameters

Momentum &

Energy

Balance

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 Tmin<4200 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

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?

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

For each species and ionization stage

Trace Species Ionization- Or split the abundance and ionization

Chromospheric Magnetic Heating Mechanism

Farley-Buneman Threshold Term

U, JHall

E,JPed

B

Uthr=Cs(1+ψ)

Prominence-Eruption-CME

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

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