  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.
