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

  title={Accurate and homogeneous abundance patterns in solar-type stars of the solar neighbourhood: a chemo-chronological analysis},
  author={R. O. da Silva and Gustavo F. Porto de Mello and A de C Milone and L. Pinheiro da Silva and L. S. Ribeiro and Helio J. Rocha-Pinto},
  journal={Astronomy and Astrophysics},
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… 
High-precision abundances of elements in solar-type stars
Aims. Previous high-precision studies of abundances of elements in solar twin stars are extended to a wider metallicity range to see how the trends of element ratios with stellar age depend on
Gaia FGK benchmark stars: abundances of α and iron-peak elements
Context. In the current era of large spectroscopic surveys of the Milky Way, reference stars for calibrating astrophysical parameters and chemical abundances are of paramount importance. Aims. We
High-precision abundances of Sc, Mn, Cu, and Ba in solar twins. Trends of element ratios with stellar age
A previous study of correlations between element abundance ratios, [X/Fe], and ages of solar twin stars is extended to include Sc, Mn, Cu, and Ba. HARPS spectra with S/N > 600 are used to derive very
Age-resolved chemistry of red giants in the solar neighbourhood
In the age of high-resolution spectroscopic stellar surveys of the Milky Way, the number of stars with detailed abundances of multiple elements is rapidly increasing. These elemental abundances are
We compile spectroscopic abundance data from 84 literature sources for 50 elements across 3058 stars in the solar neighborhood, within 150 pc of the Sun, to produce the Hypatia Catalog. We evaluate
Dynamical information along with survey data on metallicity and in some cases age have been used recently by some authors to search for candidates of stars that were born in the cluster where the Sun
On the metallicity dependence of the [Y/Mg]–age relation for solar-type stars
Several recent studies of solar twins in the solar neighbourhood have shown a tight correlation between various elemental abundances and age, in particular [Y/Mg]. If this relation is real and valid
The AMBRE Project: [Y/Mg] stellar dating calibration with Gaia
Chemical abundance dating methods open new paths for temporal evolution studies of the Milky Way stellar populations. In this paper, we use a high spectral resolution database of turn-off stars in
A PCA approach to stellar abundances I. testing of the method validity
  • Wei He, Gang Zhao
  • Physics, Geology
    Research in Astronomy and Astrophysics
  • 2019
The derivation of element abundances of stars is a key step in detailed spectroscopic analysis. A spectroscopic method may suffer from errors associated with model simplifications. We have developed
High-resolution Spectroscopic Observations of Single Red Giants in Three Open Clusters: NGC 2360, NGC 3680, and NGC 5822
Single stars in open clusters with known distances are important targets in constraining the nucleosynthesis process since their ages and luminosities are also known. In this work, we analyze a


The metallicities and abundance ratios, [X/Fe], of 12 elements—C, Na, Mg, Si, S, Ca, Ti, Cr, Ni, Y, Zr, and Ce—are determined for 14 old and 24 young metal-rich stars based on high resolution, high
Dynamical evidence of the age-metallicity relation in the Milky Way disk
Aims. We studied the relationship between the average stellar abundance of several elements and the orbital evolution of stars in the neighbourhood of the Sun. Methods. We used both observational
▪ Abstract The metallicity of stars in the Galaxy ranges from [Fe/H] = −4 to +0.5 dex, and the solar iron abundance is e(Fe) = 7.51 ± 0.01 dex. The average values of [Fe/H] in the solar neighborhood,
alpha-, r-, and s-process element trends in the Galactic thin and thick disks
From a detailed elemental abundance analysis of 102 F and G dwarf starswe present abundance trends in the Galactic thin and thick disks for 14elements (O, Na, Mg, Al, Si, Ca, Ti, Cr, Fe, Ni, Zn, Y,
Homogeneous photospheric parameters and C abundances in G and K nearby stars with and without planets
Aims. We present a determination of photospheric parameters and carbon abundances for a sample of 172 G and K dwarf, subgiant, and giant stars with and without detected planets in the solar ne
The chemical compositions of Galactic disc F and G dwarfs
Photospheric abundances are presented for 27 elements from carbon to europium in 181 F and G dwarfs from a differential local thermodynamic equilibrium (LTE) analysis of high-resolution and high
New light on stellar abundance analyses: Departures from LTE and homogeneity.
▪ Abstract The information on the chemical compositions of stars encoded in their spectra plays a central role in contemporary astrophysics. Stellar element abundances are, however, not observed: to
The Alpha Centauri Binary System: Atmospheric Parameters and Element Abundances
Context. The α  Centauri binary system, owing to its duplicity, proximity and brightness, and its components' likeness to the Sun, is a fundamental calibrating object for the theory of stellar
Manganese trends in a sample of thin and thick disk stars - The origin of Mn
Context. Manganese is an iron-peak element and although the nucleosynthesis path that leads to its formation is fairly well understood, it remains unclear which objects, SN II and/or SN Ia, that
The chemical evolution of the solar neighborhood. I. A bias-free reduction technique and data sample
The possible ways of measuring the age-metallicity relation for the galactic disk in the neighborhood of the Sun are discussed. It is shown that the use of a field star sample chosen on the basis of