  We study the s-process abundances (A > 90) at the epoch of the solar-system
formation. AGB yields are computed with an updated neutron capture network and
updated initial solar abundances. We confirm our previous results obtained with
a Galactic Chemical Evolution (GCE) model: (i) as suggested by the s-process
spread observed in disk stars and in presolar meteoritic SiC grains, a weighted
average of s-process strengths is needed to reproduce the solar s-distribution
of isotopes with A > 130; (ii) an additional contribution (of about 25%) is
required in order to represent the solar s-process abundances of isotopes from
A = 90 to 130.
  Furthermore, we investigate the effect of different internal structures of
the 13C-pocket, which may affect the efficiency of the 13C(a, n)16O reaction,
the major neutron source of the s-process. First, keeping the same 13C profile
adopted so far, we modify by a factor of two the mass involved in the pocket;
second, we assume a flat 13C profile in the pocket, and we test again the
effects of the variation of the mass of the pocket.
  We find that GCE s-predictions at the epoch of the solar-system formation
marginally depend on the size and shape of the 13C-pocket once a different
weighted range of 13C-pocket strengths is assumed. We ascertain that,
independently of the internal structure of the 13C-pocket, the missing
solar-system s-process contribution in the range from A = 90 to 130 remains
essentially the same.
