The stellar metallicity--giant planet connection

Abstract

The parent stars of the recently announced planetary system candidates are far from typical in terms of their chemical compositions. In this study we report on spectroscopic abundance analyses of ν And and τ Boo. Both stars are metal-rich relative to the Sun, with a mean [Fe/H] value near 0.25. These findings follow the trend set by two other planetary system candidates, ρ¹ 55 Cnc and 51 Peg, which also display metallicities much higher than the average for nearby dwarfs. In addition, their companions share similar orbital characteristics. Given these observations, we propose that the current metallicities of these four stars are not representative of that of the original interstellar clouds from which they formed but, rather, are the result of self-pollution during the planet formation epoch early in their histories.