A SUPER-SOLAR METALLICITY FOR STARS WITH HOT ROCKY EXOPLANETS
Journal
Date Issued
2016
Author(s)
Abstract
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, P\lt 10 days, the difference in host star metallicity is largest for hot rocky planets (\lt 1.7 {R}\oplus ), 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.
Volume
152
Issue
6
Start page
187
Issn Identifier
0004-6256
Ads BibCode
2016AJ....152..187M
Rights
open.access
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Mulders_etal2016.pdf
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Mulders et al. 2016, AJ 152, 187
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