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C II abundances in early-type stars: solution to a notorious non-LTE problem}\end{center} 

\centerline{\bf M. F. Nieva(1,2), N. Przybilla(1)
}{\footnotesize 1) Dr. Remeis Sternwarte Bamberg, Sternwartstr. 7, D-96049 Bamberg, Germany
2)Observatorio Nacional, Rua General Jose Cristino 77 CEP 20921-400, Rio de Janeiro, Brazil
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We address a long-standing discrepancy between non-LTE analyses of the prominent C II 4267 and 6578/82 A multiplets in early-type stars. A comprehensive non-LTE model atom of C II is constructed based on critically selected atomic data. This model atom is used for an abundance study of six apparently slow-rotating main-sequence and giant early B-type stars. High-resolution and high-S/N spectra allow us to derive highly consistent abundances not only from the classical features but also from up to 18 further C II lines in the visual - including two so far unreported emission features equally well reproduced in non-LTE. These results require the stellar atmospheric parameters to be determined with care. A homogeneous (slightly) sub-solar present-day carbon abundance from young stars in the solar vicinity (in associations and in the field) of log C/H +12= 8.29+/-0.03 is indicated.

{\bf Reference: 2006,ApJ, 639, L39} \\{\it Status:} Manuscript has been accepted\\ {\it Comments:} 

{\it On the web at:} {\tt http://arxiv.org/abs/astro-ph/0602342} 

{\it Preprints from:} {\tt  nieva@sternwarte.uni-erlangen.de} 
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