  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.
