Rubidium abundances are determined from the Rb 1 7800 A line via synthetic spectra for a sample of M, MS, and S giants. The Rb abundance increases with increasing s-process enrichment. A ratio Rb/Sr ≃ 0.05 is derived for the s-processed material from the He-burning shell. Thanks to the branch in the s-process path at 85Kr the Rb/Sr ratio may be used to determine the neutron density at the time of s-processing. The derived ratio is consistent with predicted neutron densities for operation of the s-process during the interpulse intervals in low-mass asymptotic giant branch (AGB) stars but clearly inconsistent with much higher neutron densities predicted for the running of the s-process in the He-shell thermal pulses of intermediate mass AGB stars and probably also of low-mass AGB stars.Zirconium isotopic abundances are determined from ZrO bandheads near 6925 Å via synthetic spectra for a sample of S stars. No evidence is found for the isotope 96Zr whose synthesis is controlled by the branch in the s-process path at 95Zr. This observation shows that the observed stars are not intermediate mass stars with massive (MC ≳ 1 Msun) cores. The absence of 96Zr sets an upper limit on the neutron density at the s-process site which is higher than and, therefore, consistent with the limit set by the Rb abundances in related stars.