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- W2274533609 abstract "We used a large sample of FGK dwarf planet-hosting stars with stellar parameters derived in a homogeneous way from the SWEET-Cat database (Santos et al. 2013) to study the relation between stellar metallicity and position of planets in the period-mass diagram. Using this large sample we show that planets orbiting metal-poor stars have longer periods than those in metal-rich systems. This trend is valid for masses at least from ≈ 10 M⊕ to ≈ 4 MJup. Moreover, Earth-like planets orbiting metal-rich stars always show shorter periods (≤20 days) than those orbiting metal-poor stars. However, in the short-period regime there are a similar number of planets orbiting metal-poor stars. Our results suggest that the planets in the P-MP diagram are evolving differently because of a mechanism that operates over a wide range of planetary masses. This mechanism is stronger or weaker depending on the metallicity of the respective system. Most probably planets in metal-poor disks form farther out from their central star and/or they form later and do not have time to migrate as far as the planets in metal-rich systems." @default.
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- W2274533609 date "2014-01-01" @default.
- W2274533609 modified "2023-09-27" @default.
- W2274533609 title "Star-planet connection through metallicity" @default.
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- W2274533609 doi "https://doi.org/10.1051/eas/1567062" @default.
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