New non-LTE calculations for C II, focusing on multiplets 6, 4267.02/4
267.27 Angstrom, and 2, 6578.03/ 6582.85 Angstrom, are presented for e
arly-B/late-O stars. The predicted strengths for these transitions, wh
ich are prominently used in abundance analysis, are weaker than previo
usly published results, and it is explicitly demonstrated that the non
-LTE line strengths have converged with respect to model atom complexi
ty. Comparison of these results to recent observations gives better ag
reement for realistic values of the microturbulent parameter. Error bo
unds for the non-LTE predictions are also provided.