A&A 439, 1137-1148 (2005)
PHOENIX model chromospheres of mid- to late-type M dwarfs B. Fuhrmeister, J. H. M. M. Schmitt and P. H. Hauschildt
Hamburger Sternwarte, University of Hamburg,
Gojenbergsweg 112, 21029 Hamburg, Germany
(Received 9 November 2004 / Accepted 28 April 2005)
We present semi-empirical model chromospheres computed with
the atmosphere code PHOENIX. The models are designed to fit
the observed spectra of five mid- to late-type M dwarfs. Next
to hydrogen lines from the Balmer series we used various metal
lines, e.g. from Fe I, for the comparison between data and models.
Our computations show that an NLTE treatment of C, N, O
impacts on the hydrogen line formation, while NLTE treatment of
less abundant metals such as nickel influences the lines
of the considered species itself. For our coolest models we
investigated also the influence of dust on the chromospheres and
found that dust increases the emission line flux.
Moreover we present an (electronically published) emission line list for
the spectral range of 3100 to 3900 and 4700 to 6800 Å for a
set of 21 M dwarfs and brown dwarfs. The line list includes the detection of the
D lines in emission for a L3 dwarf.
stars: activity --
stars: late-type --
Tables at the CDS
© ESO 2005
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