Testing planet formation theories with Giant stars

TL;DR

This paper explores how planet formation theories are informed by observations of giant stars, revealing differences from main sequence stars and suggesting complex formation mechanisms influenced by stellar mass.

Contribution

It provides new insights into planet formation around evolved giant stars, highlighting differences in metallicity and planet frequency compared to solar-type stars.

Findings

Giant stars do not show a metallicity-planet correlation.

Higher frequency and mass of planets around giant stars.

Planet formation may involve multiple mechanisms depending on stellar mass.

Abstract

Planet searches around evolved giant stars are bringing new insights to planet formation theories by virtue of the broader stellar mass range of the host stars compared to the solar-type stars that have been the subject of most current planet searches programs. These searches among giant stars are producing extremely interesting results. Contrary to main sequence stars planet-hosting giants do not show a tendency of being more metal rich. Even if limited, the statistics also suggest a higher frequency of giant planets (at least 10 %) that are more massive compared to solar-type main sequence stars. The interpretation of these results is not straightforward. We propose that the lack of a metallicity-planet connection among giant stars is due to pollution of the star while on the main sequence, followed by dilution during the giant phase. We also suggest that the higher mass and frequency of the planets are due to the higher stellar mass. Even if these results do not favor a specific formation scenario, they suggest that planetary formation might be more complex than what has been proposed so far, perhaps with two mechanisms at work and one or the other dominating according to the stellar mass. We finally stress as the detailed study of the host stars and of the parent sample is essential to derive firm conclusions.