We have updated our 1973-1990 cross section calculations by using the measured partial cross sections of the hydrogen target of the transport collaboration for beams of nuclei 10 ≤ Z ≤ 28, of the hydrogen-carbon targets of Webber et al. for beams of 5 ≤ Z ≤ 28, and of the University of Minnesota-Washington University-Caltech collaboration for beams of Fe, Kr, Ag, La, Ho, and Au nuclei. We have developed 18 modifications of equations of cross section parameters. Exact values of partial cross sections are important for evaluating the source composition of cosmic rays that have small relative abundances relative to the secondary spallation products, e.g.,13C,14N,18O,25Mg,26Mg, and 31P. The isotopic ratios 13C/12C,18O/16O,22Ne/20Ne, and (25Mg +26Mg)/24Mg are affected by the Wolf-Rayet star contributions to cosmic rays, while 14N and particularly H and He are affected by the suppression of light nuclei in cosmic rays. The abundance of P is crucial in distinguishing between the two models: (1) stellar flare versus (2) enhanced nonvolatile grain-sputtering material contribution to cosmic rays. The earlier S and T cross sections of 20Ne and 24Mg into 14N and 15N are increased by a factor of 1.5, which reduces the calculated source component of N. The earlier calculated S and T cross sections of Au (and presumably of the Pt to Pb group), into elements with ΔZ 60 above the solar system abundances.