Oxygen line formation in 3D hydrodynamical model atmospheres
| dc.creator | Asplund, M. | |
| dc.date | 2000-11-02 | |
| dc.date.accessioned | 2026-07-07T01:56:22Z | |
| dc.date.available | 2026-07-07T01:56:22Z | |
| dc.description | The formation of [O I], O I and OH lines in metal-poor stars has been studied by means of 3D hydrodynamical model atmospheres. For O I detailed 3D non-LTE calculations have been performed. While the influence of 3D model atmospheres is minor for [O I] and O I lines, the very low temperatures encountered at low metallicities have a drastic impact on the OH lines. As a result, the derived O abundances are found to be systematically overestimated in 1D analyses, casting doubts on the recent claims for a monotonic increase in [O/Fe] towards lower metallicities. | |
| dc.description | Invited talk presented at IAU General Assembly Joint Discussion 8 "Oxygen abundances in old stars and implications for nucleosynthesis and cosmology", Manchester, August 2000. The full version of the talk can be found at http://www.astro.uu.se/~martin/talks/Manchester00 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0011043 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0011043 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/1971 | |
| dc.subject | Astrophysics | |
| dc.title | Oxygen line formation in 3D hydrodynamical model atmospheres | |
| dc.type | text |