  A Massive Compact Halo Object (Macho) that lenses a background star will
magnify different parts of the rotating stellar disk by varying amounts. The
differential magnification will cause a shift in the centroid of the star's
spectral lines during the lensing event. The shift is proportional to the ratio
of the stellar radius to the projected separation of the Macho from the star.
It therefore provides a direct measure of the Einstein ring radius, and so also
a measure of the Macho's proper motion (angular speed). This measurement can
remove some of the degeneracy between mass, distance to the lens, and
transverse velocity that exists in the interpretation of results from ongoing
microlensing experiments, and is an independent test of the lensing nature of
the event. We show that using the high precision attainable by stellar radial
velocity measurements, it is possible to measure proper motions for $\sim 10\%$
of Machos that lens A-stars in the Large Magellanic Cloud (LMC), i.e.\ $\sim
7\%$ of the type of relatively high-magnification events that have been
reported to date. If this proper-motion measurement were combined with a
parallax measurement of the ``reduced velocity'', then the Macho mass,
distance, speed, and direction could each be separately determined. The shift
can be measured for $\sim 20\%$ of the A-star events generated by Machos in the
dark halo of the LMC. This in turn would provide a measurement of the fraction
of LMC vs. Galactic Macho events.
