  We use an $N$-body+smoothed particle hydrodynamics simulation of an isolated
barred galaxy to study the age dependence of bulge longitudinal proper motion
($\mu_l$) rotation curves. We show that close to the minor axis ($|l| \sim
0^\circ$) the relatively young stars rotate more rapidly than the old stars, as
found by Hubble Space Telescope in the Milky Way's (MW's) bulge. This behaviour
would be expected also if the MW were unbarred. At larger $|l|$ a different
behaviour emerges. Because younger stars trace a strong bar, their
galactocentric radial motions dominate their $\mu_l$ at $|l| \sim 6^\circ$,
leading to a reversal in the sign of $\left< \mu_l \right>$. This results in a
rotation curve with forbidden velocities (negative $\left< \mu_l \right>$ at
positive longitudes, and positive $\left< \mu_l \right>$ at negative
longitudes). The old stars, instead, trace a much weaker bar and thus their
kinematics are more axisymmetric, resulting in no forbidden velocities. We
develop metrics of the difference in the $\left< \mu_l \right>$ rotation curves
of young and old stars, and forbidden velocities. We use these to predict the
locations where rotation curve reversals can be observed by HST and the Vera
Rubin Telescope. Such measurements would represent support for the amplitude of
the bar being a continuous function of age, as predicted by kinematic
fractionation, in which the bar strength variations are produced purely by
differences in the random motions of stellar populations at bar formation.

Astrophysics of Galaxies