Gijs D. Mulders, Ilaria Pascucci, Dániel Apai, Antonio Frasca, Joanna Molenda-Zakowicz

Research output: Contribution to journalArticlepeer-review

70 Scopus citations


Host star metallicity provides a measure of the conditions in protoplanetary disks at the time of planet formation. Using a sample of over 20,000 Kepler stars with spectroscopic metallicities from the LAMOST survey, we explore how the exoplanet population depends on host star metallicity as a function of orbital period and planet size. We find that exoplanets with orbital periods less than 10 days are preferentially found around metal-rich stars ([Fe/H] ≃ 0.15 ± 0.05 dex). The occurrence rates of these hot exoplanets increases to ∼30% for super-solar metallicity stars from ∼10% for stars with a sub-solar metallicity. Cooler exoplanets, which reside at longer orbital periods and constitute the bulk of the exoplanet population with an occurrence rate of 90%, have host star metallicities consistent with solar. At short orbital periods, days, the difference in host star metallicity is largest for hot rocky planets (>1.7 R o7plus;), where the metallicity difference is [Fe/H] ≃ 0.25 ± 0.07 dex. The excess of hot rocky planets around metal-rich stars implies they either share a formation mechanism with hot Jupiters, or trace a planet trap at the protoplanetary disk inner edge, which is metallicity dependent. We do not find statistically significant evidence for a previously identified trend that small planets toward the habitable zone are preferentially found around low-metallicity stars. Refuting or confirming this trend requires a larger sample of spectroscopic metallicities.

Original languageEnglish
Article number187
JournalAstronomical Journal
Issue number6
StatePublished - Dec 2016
Externally publishedYes


  • planetary systems
  • planets and satellites: formation
  • stars: abundances


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