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We have performed a detailed abundance analysis of the content of s-processelements of two dwarf stars with suspected overabundace of those elements. Suchstars belong to a special kinematic sample of the solar neighborhood, withpeculiar kinematics and different chemical abundances when compared to "normal"disk stars. We aim to define if those stars can be identified as barium stars,based on their s-process elements abundances, and their classification, i.e.,if they share their chemical profile with strong or mild barium stars. We alsointend to shed light on the possible origins of the different kinds of bariumstars. Spectra have been taken by using the FEROS spectrograph at the 1.52mtelescope of ESO, La Silla. Abundances have been derived for 18 elements, bymatching the synthetic profile with the observed spectrum. We have found thatHD 11397 shows a mild enhancement for most of the s-process elements as well asfor some r-process elements. This star seems to share its abundance profilewith the mild Ba-stars. Although showing some slight chemical anomalies for Y,Sr, Mo, and Pb, HD 14282 depicts a chemical pattern similar to the normal starswith slight s-process enhancements.

HD 11397 and HD 14282 - Two new barium stars?