Chemical abundances of 451 stars from the HARPS GTO planet search program

Neves, V.; Santos, N. C.; Sousa, S. G.; Correia, A. C. M.; Israelian, G.

doi:10.1051/0004-6361/200811328

Cited by 155 publications

(286 citation statements)

References 37 publications

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“…The average error in the [α/Fe] ratio is 0.05 dex. We note that, in general, our derived abundances agree with the [α/Fe] presented in the literature (see Neves et al 2009;Adibekyan et al, in prep. ).…”

Section: α Element Abundancesupporting

confidence: 90%

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A newα-enhanced super-solar metallicity population

Adibekyan¹,

Santos²,

Sousa³

et al. 2011

A&A

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158

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We performed a uniform and detailed analysis of 1112 high-resolution spectra of FGK dwarfs obtained with the HARPS spectrograph at the ESO 3.6 m telescope (La Silla, Chile). Most stars have effective temperatures 4700 K ≤ T eff ≤ 6300 K and lie in the metallicity range of −1.39 ≤ [Fe/H] ≤ 0.55. Our main goal is to investigate whether there are any differences between the elemental abundance trends (especially [α/Fe] ratio) for stars of different subpopulations. The equivalent widths of spectral lines are automatically measured from HARPS spectra with the ARES code. The abundances of three α elements are determined using a differential LTE analysis relative to the Sun, with the 2010 revised version of the spectral synthesis code MOOG and a grid of Kurucz ATLAS9 atmospheres. The stars of our sample fall into two populations, clearly separated in terms of The metal-poor high-α stars (thick disk) and metal-rich high-α stars are on average older than chemically defined thin disk stars (low-α stars). The two α-enhanced families have different kinematics and orbital parameters. The metal-rich α-enhanced stars, such as thin disk stars have nearly circular orbits, close to the Galactic plane. We put forward the idea that these stars may have been formed in the inner Galactic disk, but their exact nature still remains to be clarified.

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Section: α Element Abundancesupporting

confidence: 90%

“…The method and the atomic data are the same as in Neves et al (2009) (see also Adibekyan et al, in prep.). The equivalent widths (EW) were automatically measured with the ARES 3 code (Automatic Routine for line Equivalent widths in stellar Spectra - Sousa et al 2007).…”

Section: α Element Abundancementioning

confidence: 99%

A newα-enhanced super-solar metallicity population

Adibekyan¹,

Santos²,

Sousa³

et al. 2011

A&A

Self Cite

158

214

View full text Add to dashboard Cite

show abstract

“…The same behaviour was found by Chen et al (2000) and Neves et al (2009), who suggested that SN Ia is possibly contributing. The star HD 50806 is clearly enriched in Mg (and in other elements as well) according to Fig.…”

Section: Abundance Trends As a Function Of [Fe/h]supporting

confidence: 85%

“…The overall trend of our abundance ratios as a function of the stellar metallicity normally follows what has been suggested in the literature concerning the nucleosynthetic origin of the elements and their abundance evolution in time (Chen et al 2000;Reddy et al 2003;Bensby et al 2005;Chen et al 2008;Neves et al 2009). The light metals Ca, Sc, and Ti are predominantly produced by type II Supernovae (SN II) at the beginning of the enrichment history of the Galactic disc.…”

Section: Abundance Trends As a Function Of [Fe/h]supporting

confidence: 83%

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Accurate and homogeneous abundance patterns in solar-type stars of the solar neighbourhood: a chemo-chronological analysis

Silva

Mello

Milone

et al. 2012

A&A

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Aims. We report the derivation of abundances of C, Na, Mg, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, Y, Zr, Ba, Ce, Nd, and Sm in a sample of 25 solar-type stars of the solar neighbourhood, correlating the abundances with the stellar ages, kinematics, and orbital parameters. Methods. The spectroscopic analysis, based on data of high resolution and high signal-to-noise ratio, was differential to the Sun and applied to atomic line equivalent widths supplemented by the spectral synthesis of C and C 2 features. We also performed a statistical study by using the method of tree clustering analysis, searching for groups of stars sharing similar elemental abundance patterns. We derived the stellar parameters from various criteria, with average errors of 30 K, 0.13 dex, and 0.05 dex, respectively, for T eff , log g, and [Fe/H]. The average error of the [X/Fe] abundance ratios is 0.06 dex. Ages were derived from theoretical HR diagrams and membership of the stars in known kinematical moving groups.

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Volatile and refractory abundances of F‐ and G‐type stars

et al. 2013

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We present a detailed chemical abundance analysis of a sample of F- and G-type stars. We investigate the possibility that the presence of terrestrial planets could affect the volatile-to-refractory abundance ratios. Stars with and without planets exhibit very similar abundance behaviours, either for solar twins or even when considering the whole sample of 95 solar analogs, 33 with and 62 without detected planets, in the metallicity range −0.3 < [Fe/H] < 0.5. After removing the Galactic chemical evolution effects, the small differences in the abundance patterns of stars with and without planets practically disappear and the mean volatile-to-refractory abundance ratios of the two samples are very close to solar values. If the depletion signature depends on the size of the convective zone, then stars hotter than the Sun should, in principle, show enhanced volatile-to-refractory abundance differences. Thus, we have also selected a sample of late F- and early G-type main-sequence stars with high-quality spectra. We have in total 29 planet-host stars and 32 stars without planets in the Teff range 5950–6400 K. We find very accurate Galactic chemical trends of these hotter stars that match those of solar analogs. Finally, we compare the abundance ratios of volatile and refractory elements versus the condensation temperature of this sample of main-sequence stars hotter than the Sun with respect to those of solar analogs, paying special attention to those stars containing super-Earth-like planets

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Chemical abundances of 451 stars from the HARPS GTO planet search program

Cited by 155 publications

References 37 publications

A newα-enhanced super-solar metallicity population

A newα-enhanced super-solar metallicity population

Accurate and homogeneous abundance patterns in solar-type stars of the solar neighbourhood: a chemo-chronological analysis

Volatile and refractory abundances of F‐ and G‐type stars

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