  High dispersion spectra (R>40,000) for a quite large number of stars at the
main sequence turn-off and at the base of the subgiant branch in NGC6397 and
NGC6752 were obtained with the UVES on Kueyen (VLT UT2). The [Fe/H] values we
found are -2.03+/-0.02+/-0.04 and -1.42+/-0.02+/-0.04 for NGC6397 and NGC6752
respectively, where the first error bars refer to internal errors and the
second ones to systematic errors. In both clusters the [Fe/H] obtained for
TO-stars agree perfectly (within a few per cents) with that obtained for stars
at the base of the RGB. The [O/Fe]=0.21+/-0.05 value we obtain for NGC6397 is
quite low, but it agrees with previous results obtained for giants in this
cluster; also, the star-to-star scatter in both O and Fe is very small,
indicating that this small mass cluster is chemically very homogenous. On the
other side, our results show clearly and for the first time that the O-Na
anticorrelation (up to now seen only for stars on the red giant branches of
globular clusters) is present among unevolved stars in the globular cluster
NGC6752, a more massive cluster than NGC6397. A similar anticorrelation is
present also for Mg and Al, and C and N. It is very difficult to explain the
observed Na-O, and Mg-Al anticorrelation in NGC6752 stars by a deep mixing
scenario; we think it requires some non internal mechanism.
