STAR-PLANET CONNECTION THROUGH METALLICITY

• Type: Article in International Conference Proceedings Book
• Date: 2015

Authors

Adibekyan, VZ (Author) Other; Figueira, P (Author) Other; N.C. Santos (Author) FCUP; Israelian, G (Author) Other; Mortier, A (Author) Other; Mordasini, C (Author) Other; Delgado Mena, ED (Author) FCUP; Sousa, SG (Author) FCUP; Correi, ACM (Author) Other; Oshagh, M (Author) Other

Conference proceedings International

Title: MILKY WAY UNRAVELLED BY GAIA: GREAT SCIENCE FROM THE GAIA DATA RELEASES

Pages: 351-352

Conference on the Milky Way Unravelled by Gaia: GREAT Science from the Gaia Data Releases

Barcelona, SPAIN, DEC 01-05, 2014

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Other information

Authenticus ID: P-00G-EPF

DOI: 10.1051/eas/1567062

Abstract (EN): 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 approximate to 10 M-circle plus to approximate 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.

Language: English

Type (Professor's evaluation): Scientific

No. of pages: 2