Solar radiation physical modeling srpm
This presentation is the property of its rightful owner.
Sponsored Links
1 / 10

Solar Radiation Physical Modeling (SRPM) PowerPoint PPT Presentation


  • 43 Views
  • Uploaded on
  • Presentation posted in: General

Solar Radiation Physical Modeling (SRPM). J. Fontenla June 30, 2005b. Mean Intensity. Emitted Spectra. Radiative Losses. and Net Radiative. Brackett. Atomic. Molecular. Continua. Continua. Atomic Data. Radiative Transfer. Molecular Data. Non-LTE. Molecular. Atomic.

Download Presentation

Solar Radiation Physical Modeling (SRPM)

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript


Solar radiation physical modeling srpm

Solar Radiation Physical Modeling (SRPM)

J. FontenlaJune 30, 2005b


Solar radiation physical modeling srpm

Mean Intensity

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

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

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?


H ionization and ly alpha line

H Ionization and Ly Alpha Line


V1 5 ly computed profiles

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


Trace species ionization

For each species and ionization stage

Trace Species Ionization

  • Or split the abundance and ionization


Chromospheric magnetic heating mechanism

Chromospheric Magnetic Heating Mechanism

Farley-Buneman Threshold Term

U, JHall

E,JPed

B

Uthr=Cs(1+ψ)


Prominence eruption cme

Prominence-Eruption-CME

  • 3-D non-LTE radiative transfer & MHD modeling

  • Instrumentation for observing Doppler spectra, spatial- and temporal-evolution


  • Login