The Self Absorption Curve Method for the Analysis of Emission Lines of Complex Ions as a Diagnostic of the Structure of Stellar Envelopes
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A semi-empirical method has been developed to study the emission lines of ions with complex spectra such as Fe II and Ti II, formed in many sorts of stellar envelope. Information can be obtained notably about the excitation conditions, the column density and the dimensions of the line emitting region, without making detailed model dependent complex radiative transfer computations. This method is particularly useful in the study of B[e] star envelopes.
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