Star-planet connection through metallicity. Issue 67 (17th July 2015)

• Record Type: Journal Article
• Authors: Adibekyan, V.Zh.; Figueira, P.; Santos, N.C.; Israelian, G.; Mortier, A.; Mordasini, C.; Delgado Mena, E.; Sousa, S.G.; Correi, A.C.M.; Oshagh, M.
• Editors: Walton, N.A.; Figueras, F.; Balaguer-Núñez, L.; Soubiran, C.
• Is Part Of: EAS publications series. Issue 67/68(2014)
• Page Start: 351
• Page End: 352
• Publication Date: 2015-07-17
• Subjects: Astronomy -- Periodicals; 520
• DOI: 10.1051/eas/1567062
• Languages: English
• ISSNs: 1633-4760

Abstract

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 M Jup . 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-M P 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.