  The differences between the neutron-capture element abundances of halo stars
are important to our understanding of the nucleosynthesis of elements heavier
than the iron group. We present a detailed abundance analysis of carbon and
twelve neutron-capture elements from Sr up to Pb for a peculiar halo star
G24-25 with [Fe/H] = -1.4 in order to probe its origin. The equivalent widths
of unblended lines are measured from high resolution NOT/FIES spectra and used
to derive abundances based on Kurucz model atmospheres. In the case of CH, Pr,
Eu, Gd, and Pb lines, the abundances are derived by fitting synthetic profiles
to the observed spectra. Abundance analyses are performed both relative to the
Sun and to a normal halo star G16-20 that has similar stellar parameters as
G24-25. We find that G24-25 is a halo subgiant star with an unseen component.
It has large overabundances of carbon and heavy s-process elements and mild
overabundances of Eu and light s-process elements. This abundance distribution
is consistent with that of a typical CH giant. The abundance pattern can be
explained by mass transfer from a former asymptotic giant branch component,
which is now a white dwarf.
