We describe Monte Carlo models for the dynamical evolution of the massive globular cluster 47 Tuc ( NGC 104 ) .
The code includes treatments of two-body relaxation , most kinds of 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 fairly satisfactory match to surface brightness and density profiles , the velocity dispersion profile , the luminosity function in two fields , and the acceleration of pulsars .
Our models appear to require a relatively steep initial mass function for stars above about turnoff , with an index of about 2.8 ( where the Salpeter mass function has an index of 2.35 ) , and a relatively flat initial mass function ( index about 0.4 ) for the lower main sequence .
According to the model , the current mass is estimated at 0.9 million solar masses , of which about 34 % consists of remnants .
We find that primordial binaries are gradually taking over from mass loss by stellar evolution as the main dynamical driver of the core .
Despite the high concentration of the cluster , core collapse will take at least another 20Gyr .