A thermodynamical approach to the problem of star formation, presented in a previous paper, shows how, at least when the last stages of collapse are assumed as adiabatic, the characteristics of the outcomes depend on the initial conditions (thermal and rotational energies) and on the distribution of the angular momentum among the various parts of the system. In the case of a binary outcome, the distiribution can be profitably expressed in terms of two parameters, roughly corresponding to a) the spin ratio as function of the mass ratio and b) the fraction of a.m. involved in the orbital motion. A systematic exploration of these parameters allows us to analyze the different kinds of results. In this paper we present some preliminary results, assuming that both single and binary outcomes have an equilibrium Mc Laurin ellipsoidal shape, but not taking into account the possible formation of a system star+protoplanetary disc.