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Astron. Astrophys. 325, 813-818


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On the radiative transfer in atmospheres
with randomly distributed inhomogeneities

A.G. Nikoghossian1,3, S. Pojoga2,3, and Z. Mouradian3

1Byurakan Astrophysical Observatory, 378433 Byurakan, Armenia
2Astronomical Institute of Romanian Academy, 75212 Bucharest, Romania
3Observatoire de Paris-Meudon, DASOP, F-92195 Meudon Cedex, France

Received 9 January 1997 / Accepted 25 March 1997

Abstract

We consider the problem of determining the statistical properties (intensity distribution, mean value and relative mean square deviation) of radiation which emerges from a medium with randomly distributed inhomogeneities when scattering is taken into account. The analytical formalism we propose is based on Ambartsumian's method of addition of layers. This can be applied to both local thermodynamic equilibrium (LTE) and Non-LTE cases for a wide variety of situations. A more detailed treatment of the special case of pure scattering, considered as the prototype problem for the transfer of the L FORMULA -line radiation, is given. The present investigation is assumed to apply for interpreting the spectra of various inhomogeneous structures on the Sun. It is shown in particular that some specific features of the extreme ultraviolet (EUV) spectra of solar prominences may be accounted for within the framework of the theory we propose.

Key words: radiative transfer - Sun: prominences

Send offprint requests to: Z. Mouradian


© European Southern Observatory (ESO) 1997

Online publication: September 9, 1997
Last change: April 28, 1998
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