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Star-planet connection through metallicity

Published online by Cambridge University Press:  17 July 2015

V.Zh. Adibekyan ,
P. Figueira ,
N.C. Santos ,
G. Israelian ,
A. Mortier ,
C. Mordasini ,
E. Delgado Mena ,
S.G. Sousa ,
A.C.M. Correi  and
M. Oshagh
V.Zh. Adibekyan*
Affiliation:
Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal Instituto de Astrofísica e Ciência do Espaço, Universidade do Porto, Portugal
P. Figueira
Affiliation:
Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal Instituto de Astrofísica e Ciência do Espaço, Universidade do Porto, Portugal
N.C. Santos
Affiliation:
Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal Instituto de Astrofísica e Ciência do Espaço, Universidade do Porto, Portugal Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto, Portugal
G. Israelian
Affiliation:
Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
A. Mortier
Affiliation:
SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews KY16 9SS, UK
C. Mordasini
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
E. Delgado Mena
Affiliation:
Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal Instituto de Astrofísica e Ciência do Espaço, Universidade do Porto, Portugal
S.G. Sousa
Affiliation:
Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal Instituto de Astrofísica e Ciência do Espaço, Universidade do Porto, Portugal
A.C.M. Correi
Affiliation:
Departamento de Física, I3N, Universidade de Aveiro, Portugal ASD, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, France
M. Oshagh
Affiliation:
Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal Instituto de Astrofísica e Ciência do Espaço, Universidade do Porto, Portugal
*
e-mail: [email protected]
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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.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 68: The Milky Way Unravelled by Gaia: GREAT Science from the Gaia Data Releases , 2014 , pp. 351 - 352
Copyright
© EAS, EDP Sciences, 2015

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References

Adibekyan, V.Z., Figueira, P., Santos, N.C., et al., 2013, A&A, 560, A51
Santos, N.C., Sousa, S.G., Mortier, A., et al., 2013, A&A, 556, A150