  The secular stellar mass-loss causes an amplification of the orbital
separation in fragile, common proper motion, binary systems with separations of
the order of 1000 A.U. In these systems, companions evolve as two independent
coeval stars as they experience negligible mutual tidal interactions or mass
transfer. We present models for how post-main sequence mass-loss statistically
distorts the frequency distribution of separations in fragile binaries. These
models demonstrate the expected increase in orbital seapration resulting from
stellar mass-loss, as well as a perturbation of associated orbital parameters.
Comparisons between our models and observations resulting from the Luyten
survey of wide visual binaries, specifically those containing MS and
white-dwarf pairs, demonstrate a good agreement between the calculated and the
observed angular separation distribution functions.
