  We have modeled in detail the evolution of rich open star clusters such as
the Pleiades, Praesepe and Hyades, using simulations that include stellar
dynamics as well as the effects of stellar evolution. The dynamics is modeled
via direct N-body integration, while the evolution of single stars and binaries
is followed through the use of fitting formulae and recipes. The feedback of
stellar and binary evolution on the dynamical evolution of the stellar system
is taken into account self-consistently. Our model clusters dissolve in the
tidal field of the Galaxy in a time span on the order of a billion years. The
rate of mass loss is rather constant, about 1Msun per million years. The binary
fraction at first is nearly constant in time, then increases slowly near the
end of a cluster's lifetime. For clusters which are more than about 100 million
years old the fractions of stars in the form of binaries, giants and collision
products in the inner few core radii are considerably higher than in the outer
regions, beyond the cluster's half mass radius. When stars with masses >2Msun
escape from the cluster, they tend to do so with velocities higher than
average....
  <Abstract abbreviated, read manuscript for rest>
