Hostname: page-component-cd9895bd7-dzt6s Total loading time: 0 Render date: 2024-12-26T18:40:30.507Z Has data issue: false hasContentIssue false
  • English
  • Français

Behavior of sulfur in extremely metal-poor stars

Published online by Cambridge University Press:  23 December 2005

Masahide Takada-Hidai  and
Wallace L.W. Sargent
Masahide Takada-Hidai
Affiliation:
Liberal Arts Education Center, Tokai University, Hiratsuka, Kanagawa, 259-1292 Japan email: hidai@apus.rh.u-tokai.ac.jp
Wallace L.W. Sargent
Affiliation:
Department of Astronomy, Caltech, MC 105-24, Pasadena, CA 91125, USA email: wws@astro.caltech.edu
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The LTE abundances of sulfur (S) were explored in the sample of 15 metal-poor stars with the metallicity range of −4<[Fe/H]<−1.5, based on the equivalent widths of the S I(1) 9212 and 9237 Å lines measured on high-resolution spectra, which were observed by the Keck I HIRES. Combining our results and those of Takada-Hidai et al. (2005), we found that the behavior of [S/Fe] against [Fe/H] shows a nearly flat trend in the range of metallicity down to [Fe/H]∼−4.

Keywords

Stars: abundancesstars: Population IIstars: atmospheres
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S228: From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution , May 2005 , pp. 277 - 278
Copyright
© 2005 International Astronomical Union