  All the elements heavier than Fe are produced either by slow (-s) or rapid
(-r) neutron-capture process. Neutron density prevailing in the stellar sites
is one of the major factors that determines the type of neutron-capture
processes. We present the results based on the estimates of corrected value of
absolute carbon abundance, [C/N] ratio, carbon isotopic ratio and [hs/ls] ratio
obtained from the high resolution spectral analysis of six stars that include
both CH stars and CEMP stars. All the stars show enhancement of neutron-capture
elements. Location of these objects in the A(C) vs. [Fe/H] diagram shows that
they are Group I objects, with external origin of carbon and neutron-capture
elements. Low values of carbon isotopic ratios estimated for these objects may
also be attributed to some external sources. As the carbon isotopic ratio is a
good indicator of mixing, we have used the estimates of 12C/13C ratios to
examine the occurance of mixing in the stars. While the object HD 30443 might
have experienced an extra mixing process that usually occurs after red giant
branch (RGB) bump for stars with log(L/L0) > 2.0, the remaining objects do not
show any evidence of having undergone any such mixing process. The higher
values of [C/N] ratios obtained for these objects also indicate that none of
these objects have experienced any strong internal mixing processes. Based on
the estimated abundances of carbon and the neutron-capture elements, and the
abundance ratios, we have classified the objects into different groups. While
the objects HE 0110-0406, HD 30443 and CD-38 2151 are found to be CEMP-s stars,
HE 0308-1612 and HD 176021 show characteristic properties of CH stars with
moderate enhancement of carbon. The object CD-28 1082 with enhancement of both
r- and s-process elements is found to belong to the CEMP-r/s group.
