Volume 377, Number 3, October III 2001
|Page(s)||L27 - L30|
|Published online||15 October 2001|
The interpretation of Mn II emission from late-type B stars
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, Canada N6A 3K7
Accepted: 29 August 2001
The photospheric Mnii emission lines Wahlgren & Hubrig ([CITE]) detect in the spectra of several late-type B and HgMn stars and attribute to fluorescent excitation are more naturally explained by interlocked non-LTE effects acting in a photosphere in which the manganese abundance is stratified with depth. The case is particularly strong for HD 186122 (46 Aql) and HD 179761 both of which require the manganese overabundance to be concentrated to column masses of .
Key words: line: formation / radiative transfer / stars: chemically peculiar / stars: emission-line, Be
© ESO, 2001
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