Comparing binary systems from rotating parent gas structures with different total masses

In this paper we continue the investigation reported by Arreaga-Garcia (Rev. Mex. Astron. Astrofís. 52(1):1–15, 2016) concerning the morphology of binary configurations obtained via the collapse of rotating parent gas structures with total masses in the range of MT=1 to 5M⊙. Here we extend the mass range and consider the collapse of two uniform gas clumps of MT=50 and 400M⊙, so that they also rotate rigidly in such a way that its approximate virial parameter takes the values of 0.5, 1.5, and 2.5 and their collapse is induced initially by implementing an azimuthal mass perturbation. To assess the effects of the total mass of the parent gas structure on the nature of the resulting binary configurations, we also consider the collapse of two cores of MT=1 and 5M⊙. We calculate the collapse of all these parent gas structures using three values of the ratio of thermal energy to potential energy, α, and for two values of the mass perturbation amplitude. For most of our models, we next calculate the extreme value of the ratio of rotational energy to potential energy, β, so that a model with a slightly higher β value would no longer collapse. We finally calculate the binary separations, masses and some integral properties of the binary fragments, the α_f and β_f and present them in terms of the total mass of the parent structure.