  The aim of this work is to measure the abundances of n-capture elements in a
sample of six metal-poor N-rich dwarfs that were formed in globular clusters,
and subsequently became unbound from the cluster. These N-rich stars, HD 25329,
HD 74000, HD 160617, G 24-3, G 53-41, and G 90-3, were previously studied in
Paper I. The abundances of the n-capture elements in these stars were compared
to the abundances in normal metal-poor dwarfs and in globular cluster stars in
the same metallicity range in order to find evidence of an enrichment of the
material from which these N-rich stars were formed, by the ejecta of massive
asymptotic giant branch stars (AGB) inside the cluster.The abundances of 15
elements, from Sr to Yb, were derived line by line by comparing the observed
profiles to synthetic spectra in a sample of six metal-poor N-rich dwarfs and
nine classical metal-poor dwarfs. We show that, generally speaking, the
behaviours of the intermediate metal-poor stars here studied and the extremely
metal-poor stars are very different. In particular, the scatter of the [X/Fe]
ratios is much smaller since many more stars contribute to the enrichment.Among
our six metal-poor N-rich stars, three stars (G24-3 and HD 74000 and maybe also
HD 160617) present an enrichment in elements formed by the s-process, typical
of a contribution of AGB stars, unexpected at the metallicity of these stars.
This suggests that the intracluster medium from which these stars were formed
was enriched by a first generation of massive AGB stars. Another N-rich star,
G53-41, is also rich in s-process elements, but since it is more metal-rich
this could be due to the normal galactic enrichment by low-mass AGB stars
before the formation of the cluster. In contrast, two stars (G90-3 and HD
25329) have an abundance pattern compatible with a pure r-process such as that
seen in metal-poor stars with [Fe/H]<--1.5.
