  We perform a comparative analysis of the chemical kinetics of CO and $\rm
PH_3$ in Jupiter and Saturn to assess the full set of constraints available on
the troposphere water abundance in the two giant planets. For carbon monoxide
we employ both a widely used CO kinetic scheme from Yung et al, and a newly
identified CO chemical scheme from Visscher and Moses. For $\rm PH_3$ chemical
scheme, we use the same chemical scheme as in Visscher and Fegley. Yung's
chemical scheme for CO yields a water enrichment of 0.95 - 23.0 times solar
abundance on Jupiter, and an upper limit of 14.0 for Saturn. Visscher's
chemical scheme in contrast produces a water enrichment of 0.24 - 2.6 times
solar abundance in Jupiter, and for Saturn an upper limit for water enrichment
of 8.0. From this scheme, which takes advantage of the most up-to-date
kinetics, we preclude high water enrichments on Jupiter and Saturn, and show
that the kinetics approach yields Jovian bulk abundance in which values of C/O
elevated relative to solar are admissible. Our result is consistent with recent
reinterpretation of Galileo Probe data in which Jupiter formed in a
water-depleted portion of the protoplanetary disk (Mousis et al).
