Abundances of the light elements from UV (HST) and red (ESO) spectra in the very old star HD 84937⋆
1 GEPI, Observatoire de Paris, PSL Research University, CNRS, Université Paris Diderot, Sorbonne Paris Cité, Place Jules Janssen, 92195 Meudon, France
2 SETI Institute, 189 Bernardo Ave, Suite 100, Mountain View, CA 94043, USA
3 Universidade de São Paulo, IAG, Rua do Matão 1226, Cidade Universitária, 05508-900 São Paulo, Brazil
Received: 14 November 2016
Accepted: 5 January 2017
Aims. In order to provide a better basis for the study of mechanisms of nucleosynthesis of the light elements beyond hydrogen and helium in the oldest stars, the abundances of C, O, Mg, Si, P, S, K, and Ca have been derived from UV-HST and visible-ESO high resolution spectra in the old, very metal-poor star HD 84937, at a metallicity that is 1/200 that of the Sun’s. For this halo main-sequence turnoff star, the abundance determination of P and S are the first published determinations.
Methods. The LTE profiles of the lines were computed and fitted to the observed spectra. Wherever possible, we compared the abundances derived from the UV spectrum to abundances derived from the visible or near-infrared spectra, and also corrected the derived abundances for non-LTE effects. Three-dimensional (3D) CO5BOLD model atmospheres have been used to determine the abundances of C and O from molecular CH and OH bands.
Results. The abundances of these light elements relative to iron in HD 84937 are found to agree well with the abundances of these elements in classical metal-poor stars. Our HD 84937 carbon abundance determination points toward a solar (or mildly enhanced above solar) value of [C/Fe]. The modest overabundance of the α elements of even atomic number Z, typical of halo turnoff stars, is confirmed in this example. The odd-Z element P is found to be somewhat deficient in HD 84937, at [P/Fe] = −0.32, which is again consistent with the handful of existing determinations for turnoff stars of such low metallicity. We show that the abundance of oxygen, deduced from the OH band from 3D computations, is not compatible with the abundance deduced from the red oxygen triplet. This incompatibility is explained by the existence of a chromosphere heating the shallow layers of the atmosphere where the OH band, in 3D computations, is mainly formed.
Conclusions. The abundance ratios are compared to the predictions of models of galactic nucleosynthesis and evolution.
Key words: ultraviolet: stars / stars: abundances / stars: chromospheres / Galaxy: halo / Galaxy: evolution / Galaxy: abundances
Based on observations made with the NASA/ESA Hubble Space Telescope obtained under program GO-14161 at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA) and on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere (Archives of programmes 080.D-0347(A), 082.B-0610(A), 266.D-5655(A), and 073.D-0024(A) ).
© ESO, 2017