The metal-rich nature of stars with planets

By N. C. Santos, G. Israelian, M. Mayor. 2001

368 citations recorded by the source corpus.

With the goal of confirming the metallicity "excess" present in stars with planetary-mass companions, we present in this paper a high-precision spectroscopic study of a sample of dwarfs included in the CORALIE extrasolar planet survey. The targets were chosen according to the basic criteria that 1) they formed part of a limited volume and 2) they did not present the signature of a planetary host companion. A few stars with planets were also observed and analysed; namely, HD 6434, HD 13445 (Gl 86), HD 16141, HD 17051 ( ι Hor), HD 19994, HD 22049 ( ϵ Eri), HD 28185, HD 38529, HD 52265, HD 190228, HD 210277 and HD 217107. For some of these objects there had been no previous spectroscopic studies. The spectroscopic analysis was done using the same technique as in previous work on the metallicity of stars with planets, thereby permitting a direct comparison of the results. The work described in this paper thus represents the first uniform and unbiased comparison between stars with and without planetary-mass companions in a volume-limited sample. The results show that 1) stars with planets are significantly metal-rich, and 2) that the source of the metallicity is most probably "primordial" . The results presented here may impose serious constraints on planetary system formation and evolution models.

View Paper: https://www.semanticscholar.org/paper/56a1d62c995debfe0557b6e705e9d8f6600b1999

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Citations in the corpus

Theoretical Spectra and Atmospheres of Extrasolar Giant Planets (2002, methodology): “These spectra are scaled and normalized using the measured effective temperatures and gravities of the actual stars (Santos et al. 2001; Ryan 2001).”
The Effective Temperature Scale of FGK Stars. I. Determination of Temperatures and Angular Diameters with the Infrared Flux Method (2005, unknown): “We have updated the catalog with recent spectroscopic determinations, the most important of them being Mishenina & Kov- tyukh (2001), Santos et al. (2001), Heiter & Luck (2003), Stephens & Boesgaard (2002), Takada-Hiday et al. (2002), and Yong & Lambert (2003a).”
CHARACTERIZING THE COOL KOIs. III. KOI 961: A SMALL STAR WITH LARGE PROPER MOTION AND THREE SMALL PLANETS (2012, background): “The planet-metallicity correlation was originally discovered for Sun-like F, G and K-type stars, and correlated the stellar metallicity to the likelihood of hosting a Jovian-mass planet (e.g. Santos et al. 2001; Fischer & Valenti 2005; Johnson et al. 2010a).”
THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, background): “2.1.1), a view that is supported by the well-know positive correlation of stellar [Fe/H] and the frequency of giant planets (e.g. Santos et al. 2001; Fischer & Valenti 2005).”
Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, background): “The discrepant studies are based on either excitation equilibrium for about 40 Fe I lines (Santos et al. 2001, 2004; Affer et al. 2005), excitation equilibrium for about 400 or 250 Fe I lines (Luck & Heiter 2005; Sousa et al. 2008), or on spectrum synthesis for a mixture of weak and strong lines…”
The HARPS search for southern extra-solar planets - VI. A Neptune-mass planet around the nearby M dwarf Gl 581 (2005, background): “The correlation betwen the occurence of Jupiter-mass planet and the high metalliciy of the host stars (Gonzalez, 1997; Santos et al., 2001, 2004)is another exemple.”
Tidal Dissipation in Rotating Giant Planets (2003, background): “G field-star average in the solar neighborhood (e.g., Gonzalez et al. 2001; Santos et al. 2001).”
Five New Extrasolar Planets (2005, background): “Remarkably, 20% of the most metal-rich stars, ½Fe=H > 0:3, harbor planets, while less than 3% of the metal-poor stars, ½Fe=H < 0:5, harbor giant planets (Fischer & Valenti 2005; Santos et al. 2001, 2004a; Reid 2002).”