Statistical properties of exoplanets. II. Metallicity, orbital parameters, and space velocities

By Nuno C. Santos, G. Israelian, M. Mayor, R. Rebolo, S. Observatory, S. I. D. A. D. Canarias, Spain Consejo Superior de Investigaciones Científicas, Spain. 2002

148 citations recorded by the source corpus.

In this article we present a detailed spectroscopic analysis of more than 50 extra-solar planet host stars. Stellar atmospheric parameters and metallicities are derived using high resolution and high S/N spectra. The spectroscopy results, added to the previous studies, imply that we have access to a large and uniform sample of metallicities for about 80 planet hosts stars. We make use of this sample to confirm the metal-rich nature of stars with planets, and to show that the planetary frequency is rising as a function of the (Fe/H). Furthermore, the source of this high metallicity is shown to have most probably a "primordial" source, confirming previous results. The comparison of the orbital properties (period and eccentricity) and minimum masses of the planets with the stellar properties also reveal some emerging but still not significant trends. These are discussed and some explanations are proposed. Finally, we show that the planet host stars included in the CORALIE survey have similar kinematical properties as the whole CORALIE volume-limited planet search sample. Planet hosts simply seem to occupy the metal-rich envelope of this latter population.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/6241400ad53a044ca49897a3b4887a4f06cc77b1

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In Astronomy and Astrophysics

1. Nuno C. Santos
2. M. Mayor
3. C. Mordasini
4. Debra A. Fischer
5. S. Udry
6. J. Southworth
7. Y. Alibert
8. Th. Henning

Citations in the corpus

• THE COMPOSITIONAL DIVERSITY OF EXTRASOLAR TERRESTRIAL PLANETS. I. IN SITU SIMULATIONS (2010, background): “…unless migration of the giant planets can systematically result in accretion of giant planets by the host star, our results agree with previous authors (e.g., Santos et al. 2001, 2003a, 2003b, 2005; Fischer & Valenti 2005) in finding that the observed host star enrichment is primordial in origin.”
• Spectroscopic [Fe/H] for 98 extra-solar planet-host stars. Exploring the probability of planet formation (2003, methodology): “Furthermore, it has been shown that the frequency of planetary companions is a strong function of the metal content of the star (Santos et al. 2001, 2003a; Reid 2002; Santos et al. 2003a): it is much easier to find planets around metal-rich objects.”
• Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program - Galactic stellar populations and planets (2012, background): “…ous similar studies for refractory elements (e.g. Bodaghee et al. 2003; Gilli et al. 2006; Takeda et al. 2007; Neves et al. 2009; Kang et al. 2011) and for iron (e.g. Gonzalez et al. 2001; Santos et al. 2001, 2003, 2004a, 2005; Fischer & Valenti 2005; Bond et al. 2006, 2008; Johnson et al. 2010).”
• Metallicity of M dwarfs - I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence (2005, unknown): “It is now well established that planet host stars are more metal-rich than the average solar neighbourhood population (Gonzalez 1997; Santos et al. 2001, 2003, 2004).”
• Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, background): “Such a possible absence was noted by Udry et al. (2002), Santos et al. (2003) and Fischer & Valenti (2005).”
• Lithium depletion and the rotational history of exoplanet host stars (2008, background): “As the discovery rate of exoplanets has steadily increased ov r the years, now reaching nearly 300 detections, interest hasgrown in the properties of their host stars (Santos et al. 2003; Kashyap et al. 2008).”
• Precise radial velocities of giant stars. III. Spectroscopic stellar parameters (2007, background): “…mean, median and trimean metallicity values of −0.05,+0.025 and−0.015 dex, respectively. da Silva et al. (2006) and Doellinger et al. (2007),−0.07 dex for Santos et al. (2003, 2005) and Sousa et al. (2006),−0.11 dex for Johnson et al. (2007), Valenti & Fischer (2005) and Robinson et al. (2007b), 0.”
• SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs - I. New atmospheric parameters and masses for 48 stars with planets (2013, background): “Among these, suspicions have been raised concerning the metallicityorbital period relation (e.g. Queloz et al. 2000; Sozzetti 2004; Santos et al. 2003; Beaugé & Nesvorný 2013; Dawson & Murray-Clay 2013), with hot-jupiters being often pointed out as orbiting particularly metal-rich stars (note…”
• Chemical abundances of 451 stars from the HARPS GTO planet search program - Thin disc, thick disc, and planets (2009, methodology): “Our results are also consistent with previous studies of iron abundances (e.g. Gonzalez 1998; Gonzalez et al. 2001; Laws et al. 2003; Santos et al. 2001, 2003, 2004, 2005; Fischer & Valenti 2005), as expected.”
• The missing link: A 4-day period transiting exoplanet around OGLE-TR-111 (2004, methodology): “On the summed spectra, the intensity and equivalent width of some spectral lines were analyzed to estimate the temperatur , gravity and metallicity of the primary in the manner described in Santos et al. (2003).”
• Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “7 displays three distributions: The metallicity distribution of the synthetic detectable planets, the metallicity distribution of the observational comparison sample, and the fit to the metallicity distribution of the CORALIE planet search sample (Santos et al. 2003).”
• Spectroscopic metallicities for planet-host stars: Extending the samples (2005, unknown): “Further refinements to these studies have shown that the probability of finding (and presumably forming) a planet, at least of the kind now discovered by radial-velocity surveys, is a strong function of the stellar metal content (Santos et al. 2001, 2003, 2004b; Reid 2002; Fischer & Valenti 2005).”
• Catalog of Nearby Exoplanets (2006, unknown): “…al. (2002); Pp4: Pepe et al. (2004); Pr3: Perrier et al. (2003); Q0: Queloz et al. (2000); R5: Rivera et al. (2005); Sn1: Santos et al. (2001); Sn3: Santos et al. (2003); Sn4b: Santos et al. (2004); St3: Sato et al. (2003); St5: Sato et al. (2005); Sz6: Sozzetti et al. (2006); T6: Tinney et al.…”
• The interaction of giant planets with a disc with MHD turbulence – IV. Migration rates of embedded protoplanets (2003, background): “1 I N T RO D U C T I O N The ongoing discovery of extrasolar giant planets has stimulated renewed interest in the theory of planet formation (e.g. Mayor & Queloz 1995; Marcy, Cochran & Mayor 2000; Vogt et al. 2002; Santos et al. 2003).”
• The Planet-Metallicity Correlation (2005, background): “Spectroscopic abundance analysis papers of planet-bearing stars raced alongside theory and extrasolar planet discovery papers (Fuhrmann et al. 1997, 1998; Gonzalez 1998, 1999; Gonzalez et al. 2001; Santos et al. 2000, 2003, 2004; Sadakane et al. 2002; Laws et al. 2003).”