  Collisionless N-body simulations are used in an effort to reproduce the
observed tendency of the surface brightness profile of bulges to change
progressively from a de Vaucouleurs law to an exponential, going from early to
late type spirals. A possible cause for this is the formation of the disc,
later in the history of the galaxy, and this is simulated by applying on the
N-body bulge the force field of a exponential disc whose surface density
increases with time. It is shown that [n], the index of the Sersic law that
best describes the surface brightness profile, does indeed decrease from 4 (de
Vaucouleurs law) to smaller values; this decrease is larger for more massive
and more compact discs. A large part of the observed trend of [n] with B/D
ratio is explained, and many of the actual profiles can be matched exactly by
the simulations. The correlation between the disc scalelength and bulge
effective radius, used recently to support the "secular evolution" origin for
bulges, is also shown to arise naturally in a scenario like this. This
mechanism, however, saturates at around n=2 and exponential bulges cannot be
produced; as [n] gets closer to 1, the profile becomes increasingly robust
against a disc field. These results provide strong support to the old-bulge
hypothesis for the early-type bulges. The exponential bulges, however, remain
essentially unexplained; the results here suggest that they did not begin their
lives as de Vaucouleurs spheroids, and hence were probably formed, at least in
part, by different processes than those of early type spirals.
