HD 11397 and HD 14282: two new barium stars? ^*,**

¹ IP&D, Universidade do Vale do Paraíba, Av. Shishima Hifumi, 2911, São, José dos Campos, 12244-000 SP, Brazil e-mail: pompeia@univap.br
² Centre for Astrophysics Research, STRI and School of Physics, Astronomy and Mathematics, University of Hertfordshire, Hatfield, UK e-mail: d.moreira-allen@herts.ac.uk

Received: 3 March 2008
Accepted: 27 June 2008

Abstract

Context. We have performed a detailed abundance analysis of the content of s-process elements of two dwarf stars with suspected overabundace of those elements. Such stars belong to a special kinematic sample of the solar neighborhood, with peculiar kinematics and different chemical abundances when compared to “normal” disk stars.

Aims. 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 also intend to shed light on the possible origins of the different kinds of barium stars.

Methods. Spectra have been taken by using the FEROS spectrograph at the 1.52 m telescope of ESO, La Silla. Abundances have been derived for 18 elements, by matching the synthetic profile with the observed spectrum.

Results. We have found that HD 11397 shows a mild enhancement for most of the s-process elements as well as for some r-process elements. This star seems to share its abundance profile with 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 stars with slight s-process enhancements.