Non coherent scattering in stellar atmospheres
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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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Non-Coherent Scattering in Stellar Atmospheres

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Non coherent scattering in stellar atmospheres

Non-Coherent ScatteringinStellar Atmospheres

P. Heinzel


Non coherent scattering in stellar atmospheres

S=B


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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