  We describe Monte Carlo models for the dynamical evolution of the nearby
globular cluster M4. The code includes treatments of two-body relaxation,
three- and four-body interactions involving primordial binaries and those
formed dynamically, the Galactic tide, and the internal evolution of both
single and binary stars. We arrive at a set of initial parameters for the
cluster which, after 12Gyr of evolution, gives a model with a satisfactory
match to the surface brightness profile, the velocity dispersion profile, and
the luminosity function in two fields. We describe in particular the evolution
of the core, and find that M4 (which has a classic King profile) is actually a
post-collapse cluster, its core radius being sustained by binary burning. We
also consider the distribution of its binaries, including those which would be
observed as photometric binaries and as radial-velocity binaries. We also
consider the populations of white dwarfs, neutron stars, black holes and blue
stragglers, though not all channels for blue straggler formation are
represented yet in our simulations.
