Spectral line formation in YY Orionis envelopes

Mathematics – Probability

Scientific paper

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Line Spectra, Protostars, Radiative Transfer, Stellar Envelopes, Stellar Models, Stellar Spectra, Absorption Spectra, Density Distribution, Emission Spectra, Probability Density Functions, Stellar Atmospheres, T Tauri Stars, Temperature Distribution

Scientific paper

The escape probability method for treating the transfer of line radiation in a moving atmosphere is used to calculate line profiles of a two-level atom in a collapsing protostar envelope. It is found that YY Orionis profiles can be reproduced for a fairly narrow range of the parameters, the values of which are in good agreement with the computed properties of nonrotating low mass protostars. From the variations of the profile shape for various temperature and density distributions, it is concluded that inhomogeneities in the infalling matter, leading to the appearance of a secondary emission component inside the redward displaced absorption feature, might be responsible for the observed short time-scale variations of the profiles.

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