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We study the effect pre-main sequence circumstellar disks have on the dynamical evolution of a small cluster of protostars formed by 'prompt initial fragmentation'. In particular we investigate the effect star-disk interactions have on the resulting mass components of the central binary formed due to gravitational disintegration of the cluster. Our simulations without disks are in good agreement with previous work in that we find the central binary in general contained the two most massive stars in the cluster. For our star disk simulations we varied a number of parameters (disk mass,disk radius, disk mass relation to stellar mass) and employed various interaction criteria in order to examine the sensitivity of our results on the model chosen. In general, we find that circumstellar disks have little effect on the mass pairings of the central binary as the gravitational interactions between the protostars dominate over any star-disk effect. However the presence of disks can often lead to the formation of a second binary.
