The stationary r -process as described by the B FH paper was first demonstrated in a time-dependent calculation at Caltech by Phillip A. Seeger, William A. Fowler and Donald D. Clayton, who found that no single temporal snapshot matched the solar r -process abundances, but, that when superposed, did achieve a successful characterization of the r -process abundance distribution. Shorter-time distributions emphasize abundances at atomic weights less than A = 140, whereas longer-time distributions emphasized those at atomic weights greater than A = 140. Subsequent treatments of the r -process reinforced those temporal features. Seeger et al. were also able to construct more quantitative apportionment between s -process and r -process of the abundance table of heavy isotopes, thereby establishing a more reliable abundance curve for the r -process isotopes than B FH had been able to define. Today, the r -process abundances are determined using their technique of subtracting the more reliable s -process isotopic abundances from the total isotopic abundances and attributing the remainder to r -process nucleosynthesis. That r -process abundance curve (vs. atomic weight) has provided for many decades the target for theoretical computations of abundances synthesized by the physical r -process.