  We try to understand the s- and r-process elements vs Ti/Fe plots derived by
Jehin et al. (1999) for mildly metal-poor stars within the framework of the
analytical semi-empirical models for these elements by Pagel & Tautvaisiene
(1995, 1997). Jehin et al. distinguished two Pop II subgroups: IIa with
alpha/Fe and s-elements/Fe increasing together, which they attribute to pure
SNII activity, and IIb with constant alpha/Fe and a range in s/Fe which they
attribute to a prolonged accretion phase in parent globular clusters. However,
their sample consists mainly of thick-disk stars with only 4 clear halo
members, of which two are `anomalous' in the sense defined by Nissen & Schuster
(1997). Only the remaining two halo stars (and one in Nissen & Schuster's
sample) depart significantly from Y/Ti (or s/alpha) ratios predicted by our
model.
