• DOI:10.1051/0004-6361:20047060
• Corpus ID: 12174134

The age of the Galactic thin disk from Th/Eu nucleocosmochronology. I. Determination of [Th/Eu] abundance ratios

@article{Peloso2005TheAO,
  title={The age of the Galactic thin disk from Th/Eu nucleocosmochronology. I. Determination of [Th/Eu] abundance ratios},
  author={E. F. del Peloso and L. Pinheiro da Silva and G. F. Porto de Mello Observatorio NacionalMCT and R. D. Janeiro and Brazil. and Observatorio do ValongoUFRJ},
  journal={Astronomy and Astrophysics},
  year={2005},
  volume={434},
  pages={275-300}
}

• E. F. D. Peloso, L. D. Silva, +3 authors Observatorio do ValongoUFRJ
• Published 25 November 2004
• Physics
• Astronomy and Astrophysics

The purpose of this work is to resume investigation of Galactic thin disk dating using nucleocosmochronology with Th/Eu stellar abundance ratios, a theme absent from the literature since 1990. A stellar sample of 20 disk dwarfs/subgiants of F5 to G8 spectral types with −0.8 ≤ (Fe/H) ≤ +0.3 was selected. In stars with such spectral types and luminosity classes, spectral synthesis techniques must be employed if we wish to achieve acceptably accurate results. An homogeneous, self-consistent set of atmospheric parameters was determined. Effective temperatures were determined from photometric calibrations and Hα profile fitting; surface gravities were obtained from Teff, stellar masses and luminosities; microturbulence velocities and metallicities were obtained from detailed, differential spectroscopic analysis, relative to the Sun, using equivalent widths of Fe  and Fe  lines. Chemical abundances of the elements that contaminate the Th and Eu spectral regions (Ti, V, Cr, Mn, Co, Ni, Ce, Nd, and Sm) were determined through spectroscopic analysis. Abundance uncertainties were thoroughly scrutinised, their average value - (0.10 ± 0.02) dex - being found to be satisfactorily low. Eu and Th abundances were determined by spectral synthesis of one Eu  line (4129.72 A) and one Th  line (4019.13 A), taking into account the detailed hyperfine structures of contaminating Co lines, as well as the hyperfine structure and isotope shift of the Eu line. Comparison of our abundances with literature data shows that our results exhibit a similar behaviour, but a considerably lower scatter (36% lower for Eu, and 61% lower for Th). The (Th/Eu) abundance ratios thus obtained were used, in the second paper of this series, to determine the age of the Galactic disk.