HD 11397 and HD 14282 - Two new barium stars?

TL;DR

This study analyzes the s-process element abundances in two dwarf stars to determine if they are barium stars and explores their possible origins, revealing one as a mild barium star and the other as chemically similar to normal stars.

Contribution

It provides detailed abundance profiles for two stars, classifying one as a mild barium star and offering insights into the origins of different barium star types.

Findings

HD 11397 shows mild s-process and some r-process enhancements.

HD 14282 has a chemical pattern similar to normal stars with slight s-process enhancements.

One star is identified as a mild barium star, the other as chemically normal.

Abstract

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