  Intermediate mass stellar evolution tracks from the main sequence to the tip
of the AGB for five initial masses (2 to 6Msun) and metallicity Z=0.0001 have
been computed. The detailed 1D structure and evolution models include
exponential overshooting, mass loss and a detailed nucleosynthesis network with
updated nuclear reaction rates. The network includes a two-particle heavy
neutron sink for approximating neutron density in the He-shell flash. It is
shown how the neutron-capture nucleosynthesis is important in models of very
low metallicity for the formation of light neutron-heavy species, like sodium
or the heavy neon and magnesium isotopes. The models have high resolution, as
required for modeling the third dredge-up. All sequences have been followed
from the pre-main sequence to the end of the AGB when all envelope mass is
lost. Detailed structural and chemical model properties as well as yields are
presented. This set of stellar models is based on standard assumptions and
updated input physics. It can be confronted with observations of
extremely-metal poor stars and may be used to assess the role of AGB stars in
the origin of abundance anomalies of some Globular Cluster members of
correspondingly low metallicity.
