  Two stellar-dynamical models of binary-rich embedded proto-Orion-Nebula-type
clusters that evolve to Pleiades-like clusters are studied with an emphasis on
comparing the stellar mass function with observational constraints. By the age
of the Pleiades (about 100 Myr) both models show a similar degree of mass
segregation which also agrees with observational constraints. This thus
indicates that the Pleiades is well relaxed and that it is suffering from
severe amnesia. It is found that the initial mass function (IMF) must have been
indistinguishable from the standard or Galactic-field IMF for stars with mass m
< 2 Mo, provided the Pleiades precursor had a central density of about 10^4.8
stars/pc^3. A denser model with 10^5.8 stars/pc^3 also leads to reasonable
agreement with observational constraints, but owing to the shorter relaxation
time of the embedded cluster it evolves through energy equipartition to a
mass-segregated condition just prior to residual-gas expulsion. This model
consequently looses preferentially low-mass stars and brown dwarfs (BDs), but
the effect is not very pronounced. The empirical data indicate that the
Pleiades IMF may have been steeper than Salpeter for stars with m > 2 Mo.
