Chemical abundances of planet-host stars: Results for alpha and Fe-group elements

TL;DR

This study compares chemical abundances of alpha and Fe-group elements in stars with and without giant planets, finding mostly similar trends and slight differences in some elements, and providing detailed galactic chemical evolution insights.

Contribution

It offers a comprehensive analysis of element abundances in planet-hosting stars versus non-hosts, with unprecedented detail at high metallicities.

Findings

No significant abundance differences between planet hosts and non-hosts for most elements.

Slight variations in V, Mn, Ti, and Co between the two groups.

Detailed galactic chemical evolution trends at high [Fe/H].

Abstract

In this paper, we present a study of the abundances of Si, Ca, Sc, Ti, V, Cr, Mn, Co, and Ni in a large set of stars known to harbor giant planets, as well as in a comparison sample of stars not known to have any planet ary-mass companions. We have checked for possible chemical differences between planet hosts and field stars without known planets. Our results show that overall, and for a given value of [Fe/H], the abundance trends for the planet hosts are nearly indistinguishable from those of the field stars. In general, the trends show no discontinuities,and the abundance distributions of stars with giant planets are high [Fe/H] extensions to the curves traced by the field dwarfs without planets. The only elements that might present slight differences between the two groups of stars are V, Mn, and to a lesser extent Ti and Co. We also use the available data to describe galactic chemical evolution trends for the elements studied. When comparing the results with former studies, a few differences emerge for the high [Fe/H] tail of the distribution, a region that is sampled with unprecedented detail in our analysis.