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Star-planet connection through metallicity

  • V.Zh. Adibekyan (a1) (a2), P. Figueira (a1) (a2), N.C. Santos (a1) (a2) (a3), G. Israelian (a4), A. Mortier (a5), C. Mordasini (a6), E. Delgado Mena (a1) (a2), S.G. Sousa (a1) (a2), A.C.M. Correi (a7) (a8) and M. Oshagh (a1) (a2)...

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.

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[1]1Adibekyan, V.Z., Figueira, P., Santos, N.C., et al., 2013, A&A, 560, A51
[2]2Santos, N.C., Sousa, S.G., Mortier, A., et al., 2013, A&A, 556, A150

Star-planet connection through metallicity

  • V.Zh. Adibekyan (a1) (a2), P. Figueira (a1) (a2), N.C. Santos (a1) (a2) (a3), G. Israelian (a4), A. Mortier (a5), C. Mordasini (a6), E. Delgado Mena (a1) (a2), S.G. Sousa (a1) (a2), A.C.M. Correi (a7) (a8) and M. Oshagh (a1) (a2)...

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