The interpretation of Mn II emission from late-type B stars

Details The interpretation of Mn II emission from late-type B stars The interpretation of Mn II emission from late-type B stars

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...377l..27s&link_type=abstract

Astronomy and Astrophysics, v.377, p.L27-L30 (2001)

Astronomy and Astrophysics

Astrophysics

8

Line: Formation, Radiative Transfer, Stars: Chemically Peculiar, Emission-Line, Be

Scientific paper

The photospheric Mn Ii emission lines Wahlgren & Hubrig (\cite{wh2000}) 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 log (m)< ~-1.5.

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