  Barium stars are one of the important probes to understand the origin and
evolution of slow neutron-capture process elements in the Galaxy. These are
extrinsic stars, where the observed s-process element abundances are believed
to have an origin in the now invisible companions that produced these elements
at their Asymptotic Giant Branch phase of evolution. We have attempted to
understand the s-process nucleosynthesis, as well as the physical properties of
the companion stars through a detailed comparison of observed elemental
abundances of 10 barium stars with the predictions from AGB nucleosynthesis
models, FRUITY. For these stars, we have presented estimates of abundances of
several elements, C, N, O, Na, Al, $\alpha$-elements, Fe-peak elements and
neutron-capture elements Rb, Sr, Y, Zr, Ba, La, Ce, Pr, Nd, Sm and Eu. The
abundance estimates are based on high resolution spectral analysis.
Observations of Rb in four of these stars have allowed us to put a limit to the
mass of the companion AGB stars. Our analysis clearly shows that the former
companions responsible for the surface abundance peculiarities of these stars
are low-mass AGB stars. Kinematic analysis have shown the stars to be members
of Galactic disk population.
