The rise and fall of the NaMgAl stars
1997 (English)In: ASTRONOMY AND ASTROPHYSICS, ISSN 0004-6361, Vol. 327, no 2, 587-597 p.Article in journal (Refereed) Published
We have made new abundance determinations for a sample of NaMgAl stars. These stars, which are a subgroup of the nearby metal-rich field F and G disk dwarfs, were first identified by Edvardsson et al. (1993) on the basis of their apparent enrichment in Na, Mg and Al relative to other elements. The discovery of a planetary companion to the nearby solar type star 51 Peg (Mayor & Queloz 1995) combined with Edvardsson et al.'s earlier identification of 51 Peg as a NaMgAl star highlighted the group's potential importance. Our new analysis, which uses new spectra of higher resolution and better wavelength coverage than the analysis of Edvardsson et al., shows that the Na, Mg and Al abundances of the NaMgAl stars are indistinguishable from those of non-NaMgAl stars with otherwise similar properties. The group thus appears to be spurious.
Our study, which includes 51 Peg, also provides the most complete set of abundances for this star available to date. The new Fe abundance, [Fe/H] = +0.20 +- 0.07, of 51 Peg confirms earlier measurements of its metal richness. Abundances for 19 other elements, including C, N and O, reveal a fairly uniform enrichment similar to that of Fe and show no evidence of abnormality compared to other metal rich stars of similar spectral type.
Place, publisher, year, edition, pages
1997. Vol. 327, no 2, 587-597 p.
stars: abundances; stars: fundamental parameters; galaxy: abundances; galaxy: evolution
IdentifiersURN: urn:nbn:se:uu:diva-85330OAI: oai:DiVA.org:uu-85330DiVA: diva2:113238
Addresses: Tomkin J., Lambert D.L.: UNIV TEXAS, MCDONALD OBSERV, AUSTIN, TX 78712. UNIV TEXAS, DEPT ASTRON, AUSTIN, TX 78712.2005-04-282005-04-282011-01-15