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 \pm 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 .