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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

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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
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