Chemical abundances of 451 stars from the HARPS GTO planet search program - Thin disc, thick disc, and planets

By V. Neves, Nuno C. Santos, Sérgio F. Sousa, A. Correia, G. Israelian. 2009

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We present a uniform study of the chemical abundances of 12 elements (Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Na, Mg, and Al) derived from the spectra of 451 stars observed as part of one of the HARPS GTO planet search programs. Sixty eight of these are planetbearing stars. The main goals of our work are: i) the investigation of possible differences between the abundances of stars with and without planets; ii) the study of the possible differences in the abundances of stars in the thin and the thick disc. We confirm that there is a systematically higher metallicity in planet host stars, when compared to non planet-hosts, common to all studied species. We also found that there is no difference in the galactic chemical evolution trends of the stars with and without planets. Stars that harbour planetary companions simply appear to be in the high metallicity tail of the distribution. We also confirm that Neptunian and super-Earth class planets may be easier to find at lower metallicities. A statistically significative abundance difference between stars of the thin and the thick disc was found for [Fe/H] < 0. However, the populations from the thick and the thin disc cannot be clearly separated.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/af9118f727080ff78981dfb3d9e659cb13ad894f

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Citations in the corpus

A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA (2013, background): “…(iv) a spatial association of the flatter area with gas located in the thick disk, which is known to have different metallicity patterns (e.g., Neves et al. 2009; Ishigaki et al. 2012); (v) a plateau of the gas abundance in the intergalactic medium due to the cosmological evolution of…”
The Gaia-ESO Survey: the analysis of high-resolution UVES spectra of FGK-type stars (2014, methodology): “Individual abundances are derived using the same tools and methodology as described above, but using the 2010 version of MOOG (see Neves et al. 2009; Adibekyan et al. 2012, for details).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, background): “Apart from spectroscopically determinedTeff and [Fe/H], all these surveys provideα abundances: Si and Ti in the case of Valenti & Fischer (2005), and Mg, Si, Ca, Ti for the other two studies (for the Sousa et al. 2008 sample the abundances are given in the companion paper of Neves et al. 2009, N09).”
STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG (2014, methodology): “However, the dominant survey was different in the cases of different elements (i.e. Neves et al. (2009) for Mg, Valenti & Fischer (2005) for Si).”
The HARPS search for Earth-like planets in the habitable zone - I. Very low-mass planets around HD 20794, HD 85512, and HD 192310 (2011, background): “We only comment that for the K5V dwarf HD 85512 the stellar parameters derived in Sousa et al. may be affected by systematic errors (see e.g. Neves et al. 2009), given the late spectral type of the star.”
PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER (2011, background): “Another potential bias stems from the metallicity gradient as a function of height above the galactic plane (Bensby et al. 2007; Neves et al. 2009).”
Accurate abundance patterns of solar twins and analogs - Does the anomalous solar chemical composition come from planet formation? (2009, result): “When compared to the abundance trends for Galactic thin-disk stars published elsewhere (e.g., Bensby et al. 2005; Reddy et al. 2006; Takeda 2007; Neves et al. 2009), we notice that the slopes and relativ scatter (between different elements) are compatible with our results (all but the two most…”
AN ANCIENT EXTRASOLAR SYSTEM WITH FIVE SUB-EARTH-SIZE PLANETS (2015, methodology): “…whether or not exoplanet-host stars differ from stars without planets in their content of individual heavy elements showed no significant difference between the two populations (Fischer & Valenti 2005; Takeda 2007; Neves et al. 2009; Delgado Mena et al. 2010; González Hernández et al. 2013).”
Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program - Galactic stellar populations and planets (2012, methodology): “…spaces, which agrees well with previous 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, 2004, 2005; Fischer & Valenti 2005; Bond et…”
High-precision abundances of elements in solar twin stars - Trends with stellar age and elemental condensation temperature (2015, background): “Furthermore, the lowest Ni/Fe and Na/Fe ratios are found among 5 For the solar twin stars studied, abundance ratios derived from HARPS spectra by Neves et al. (2009) show in fact correlated variations in [Ni/Fe] and [Na/Fe] similar to Fig.”