  We present stellar yields computed from detailed models of intermediate mass
asymptotic giant branch stars of low metallicity. In this work, the whole main
microphysics inputs have been updated, and in particular alpha-enhancement is
explicitly taken into account both in the opacities and equation of state. The
target of this work is to provide a basis to test the reliability of the AGB
self-enrichment scenario for Globular Clusters of intermediate metallicity.
These Globular Clusters exhibit well defined abundance patterns, which have
often been interpreted as a consequence of the pollution of the interstellar
medium by the ejecta of massive AGBs. We calculated a grid of intermediate mass
models with metallicity Z=0.001; the evolutionary sequences are followed from
the pre-Main sequence along the whole AGB phase. We focus our attention on
those elements largely studied in the spectroscopic investigations of Globular
Clusters stars, i.e. oxygen, sodium, aluminum, magnesium and fluorine.} The
predictions of our models show an encouraging agreement with the demand of the
self-enrichment scenario for what concerns the abundances of oxygen, aluminum,
fluorine and magnesium. The question of sodium is more tricky, due to the large
uncertainties of the cross-sections of the Ne-Na cycle. The present results
show that only a relatively small range of initial masses (M=5,6 solar masses)
can be responsible for the self enrichment.
