Non coherent scattering in stellar atmospheres
Download
1 / 42

Non-Coherent Scattering in Stellar Atmospheres - PowerPoint PPT Presentation


  • 116 Views
  • Uploaded on

Non-Coherent Scattering in Stellar Atmospheres. P. Heinzel. S=B. Multilevel atoms. Special new problems Absorption profile for a two-level atom known, f 1 =f M (Voigt fct) For a three-level atom, transition 2 -> 3, NOT known since f 2 will differ from f M due to a selective absorption

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about ' Non-Coherent Scattering in Stellar Atmospheres' - takoda


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
Non coherent scattering in stellar atmospheres

Non-Coherent ScatteringinStellar Atmospheres

P. Heinzel



Multilevel atoms
Multilevel atoms

Special new problems

Absorption profile for a two-level atom known, f1=fM (Voigt fct)

For a three-level atom, transition 2 -> 3, NOT known since f2 will differ

from fM due to a selective absorption

Emission profile for transition 3 -> 2 also NOT known, f3 also differs from

fM

For CRD we have fi=fM


Natural population
Natural population

  • Spontaneous emission

  • Inellastic collisions

  • Ionization and recombination

  • Excitation by frequency-independent radiation

    -> i *


Generalized redistribution functions
Generalized redistribution functions

Finite number of atomic levels -> finite number of non-Markovian radiation processes

1*=>2=>3 … =>n->I

GRF describe photon correlations in each sequence of

consecutive radiation transitions of the atom that starts from naturally populated initial level


Emission in the transition 3 1 l
Emission in the transition 3->1 (L)

  • ->3*->1 prob{->3*}

  • 1*=>3->1 prob{1*=>3}

  • ->2*=>3->1 prob{->2*=>3}

  • 1*=>2=>3->1 prob{1*=>2=>3}


Absorption in the transition 2 3 h
Absorption in the transition 2=>3 (H)

  • -> 2* => 3 prob{->2*}

  • 1*=>2=>3 prob{1*=>2}


Solution of the transfer problem
Solution of the transfer problem

  • Generalized redistribution functions

  • Multilevel cases

  • General approach

  • Solution of the transfer problem

    (2-level atom, ETLA, ETLA+LINEAR, MALI)

  • Applications


ad