  We present an elemental-abundance analysis, in the near-ultraviolet (NUV)
spectral range, for the bright carbon-enhanced metal-poor (CEMP) stars HD196944
(V = 8.40, [Fe/H] = -2.41) and HD201626 (V = 8.16, [Fe/H] = -1.51), based on
data acquired with the Space Telescope Imaging Spectrograph (STIS) on the
Hubble Space Telescope. Both of these stars belong to the sub-class CEMP-s, and
exhibit clear over-abundances of heavy elements associated with production by
the slow neutron-capture process. HD196944 has been well-studied in the optical
region, but we are able to add abundance results for six species (Ge, Nb, Mo,
Lu, Pt, and Au) that are only accessible in the NUV. In addition, we provide
the first determination of its orbital period, P=1325 days. HD201626 has only a
limited number of abundance results based on previous optical work -- here we
add five new species from the NUV, including Pb. We compare these results with
models of binary-system evolution and s-process element production in stars on
the asymptotic giant branch, aiming to explain their origin and evolution. Our
best-fitting models for HD 196944 (M1,i = 0.9Mo, M2,i = 0.86Mo, for
[Fe/H]=-2.2), and HD 201626 (M1,i = 0.9Mo , M2,i = 0.76Mo , for [Fe/H]=-2.2;
M1,i = 1.6Mo , M2,i = 0.59Mo, for [Fe/H]=-1.5) are consistent with the current
accepted scenario for the formation of CEMP-s stars.
