Although the abundances of heavy s-process elements could not be estimated, the upper limits of the abundances of Ce, Nd do demonstrate the lighter s-process elements are more enhanced even in EHe stars. It is generally acknowledged that 13 C(α, n) 16 O is the main source of neutrons to run the s-processing in the He-burning shells of intermediate-mass AGB stars. Sufficient amounts of 13 C are to be generated by slow mixing of protons into the 12 C rich intershell regions to generate neutrons. The neutron irradiation occurs in radiative conditions. The heavier the neutron flux the greater is the abundance of heavies relative to light s-process elements. Busso et al. (2001)  the distribution of the ratio of heavy s-process celements (hs) to the light s-process (ls) elements with respect to metallicity to characterize various parameters of neutron exposures during the third dredgeup phase in AGB stars eg. mass of 13 C pocket in the inter shell regions. Reddy et al. (2002) showed that the variation of the [hs/ls] with respect to metallicity in post -AGB stars (that went through third dredgeup) is characterized by a model ST/1.5 of Busso et al. (2001). 4 ) shows that the enhancements are positive and both show a similar range in their abundances. We compared the run of the ratio of [ls/hs] for RCBs and EHes with respect to the metallicity parameter [M] . The estimates for EHes are based on the upper limits for the heavy s-process elements and includes **data** from our ongoing analysis of the HST UV spectra. Estimates of U Aqr and the born again giant, Sakurai's object (during May -Oct 1996) are also included for comparison. Both the groups RCBs and EHes blend together emphasizing the similarity in their ls/hs ratios. that shown by post-AGB stars. It also, probably, suggests the s-processing in RCBs and EHes is not a result of the third dredgeup and could have happened when the stars passed through a second AGB phase (presumably).