High precision cross sections estimates are crucial to help infer the source abundance of elements and isotopes that have large secondary components in the arriving cosmic-ray abundances, e.g., N, Na, Al and P. We propose here correction factors to further refine our recent semiempirical cross sections estimates. Factors for
elements that are nearly purely secondary, e.g, B and F, are also proposed for improved propagation calculations.
We also point to some inconsistencies in the measured cross sections. The nucleus-nucleus component, including scaling factors, as well as a non-nuclear contribution to the inelastic cross section therein are also discussed
