  We examine the possibility of observing gravitational lensing in the weak
deflection regime by the supermassive black hole in the center of the galaxy
M31. This black hole is significantly more massive than the black hole in the
center of our Galaxy qualifying itself as a more effective lens. However, it is
also more distant and the candidate stellar sources appear consequently
fainter. As potential sources we separately consider stars belonging to the
bulge, to the disk, to the triple nucleus formed by P1+P2 and by the recently
discovered inner cluster P3. We calculate the number of simultaneously lensed
stars at a given time as a function of the threshold magnitude required for the
secondary image. For observations in the K-band we find 1.4 expected stars
having secondary images brighter than K=24 and 182 brighter than K=30. For
observations in the V-band we expect 1.3 secondary images brighter than V=27
and 271 brighter than V=33. The bulge stars have the highest chance to be
lensed by the supermassive black hole, whereas the disk and the composite
nucleus stars contribute by 10% each. The typical angular separation of the
secondary images from the black hole range from 1 mas to 0.1''. For each
population we also show the distribution of the lensed sources as a function of
their distance and absolute magnitude, the expected angular positions and
velocities of the generated secondary images, the rate and the typical duration
of the lensing events.
