On the Origin of Sulfur
| dc.creator | Ryde, Nils | |
| dc.creator | Lambert, David L. | |
| dc.date | 2005-10-05 | |
| dc.date.accessioned | 2026-07-07T06:20:57Z | |
| dc.date.available | 2026-07-07T06:20:57Z | |
| dc.description | We present our work on the halo evolution of sulfur, based on observations of the S I lines around 9220 A for ten stars for which the S abundance was obtained previously from much weaker S I lines at 8694 A. We cannot confirm the rise and the high [S/Fe] abundances for low [Fe/H], as claimed in the literature from analysis of the 8694 A lines. The reasons for claims of an increase in [S/Fe] with decreasing [Fe/H] are probably twofold: uncertainties in the measurements of the weak 8694 A lines, and systematic errors in metallicity determinations from Fe I lines. The near-infrared sulfur triplet at 9212.9, 9228.1, and 9237.5 A are preferred for an abundance analysis of sulfur for metal-poor stars. Our work was presented in full by Ryde & Lambert (2004). | |
| dc.description | In conference proceedings: Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis in honor of David L. Lambert | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0510136 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0510136 | |
| dc.identifier | ASP Conference Series, Vol. 336, p 355 (2005) | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/95454 | |
| dc.subject | Astrophysics | |
| dc.title | On the Origin of Sulfur | |
| dc.type | text |