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Searching for the signatures of terrestial planets in solar analogs

J. I. GonzŠlez HernŠndez, G. Israelian, N. C. Santos, S. G. Sousa, E. Delgado Mena, V. Neves, S. Udry

We present a fully differential chemical abundance analysis using very highresolution (λ/δλ ≳ 85,000) and very high signal-to-noise (S/N ∼ 800 on average) HARPS and UVES spectra of 7 solar twins and 95 solar analogs, 24 are planet hosts and 71 are stars without detected planets. The whole sample of solar analogs provide very accurate Galactic chemical evolution trends in the metalliciy range -0.3 < [Fe/H] < 0.5. Solar twins with and without planets show similar mean abundance ratios. We have also analysed a sub-sample of 28 solar analogs, 14 planet hosts and 14 stars without known planets, with spectra at S/N ∼ 850 on average, in the metallicity range 0.14 < [Fe/H] < 0.36 and find the same abundance pattern for both samples of stars with and without planets. This result does not depend on either the planet mass, from 7 Earth masses to 17.4 Jupiter masses, or the orbital period of the planets, from 3 to 4300 days. In addition, we have derived the slope of the abundance ratios as a function of the condensation temperature for each star and again find similar distributions of the slopes for both stars with and without planets. In particular, the peaks of these two distributions are placed at a similar value but with opposite sign as that expected from a possible signature of terrestial planets. In particular, two of the planetary systems in this sample, containing each of them a Super-Earth like planet, show slope values very close to these peaks which may suggest that these abundance patterns are not related to the presence of terrestial planets.

planetary systems – stars: abundances – stars: atmospheres – stars: formation – stars: fundamental parameters

The Astrophysical Journal
Volume 720, Page 1592
2010 August

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Instituto de Astrof√≠sica e Ci√™ncias do Espa√ßo Universidade do Porto Faculdade de Ciências da Universidade de Lisboa Funda√ß√£o para a Ci√™ncia e a Tecnologia
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