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

## TL;DR

This study investigates how the total mass of rotating parent gas structures influences the formation and properties of binary systems resulting from their collapse, extending previous work to larger mass ranges.

## Contribution

It extends prior research by analyzing binary formation from higher mass gas structures (50 and 400 M$_{ ext{sun}}$) and assesses the impact of mass, rotation, and perturbations on binary properties.

## Key findings

- Binary separations scale with parent mass
- Higher mass structures produce more massive binaries
- Collapse stability depends on the $eta$ parameter

## Abstract

In this paper we continue the investigation reported by \cite{RMAA} concerning the morphology of binary configurations obtained via the collapse of rotating parent gas structures with total masses in the range of M$_T$= 1 to 5 M$_{\odot}$. Here we extend the mass range and consider the collapse of two uniform gas clumps of M$_T$= 50 and 400 M$_{\odot}$, so that they also rotates 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 M$_T$= 1 and 5 M$_{\odot}$. We calculate the collapse of all these parent gas structures using three values of the ratio of thermal energy to potential energy and for two values of the mass perturbation amplitude. We next calculate the binary separations, masses and integral properties of the binary fragments and present them in terms of the total mass of the parent structure. For most of our models, we finally calculate the $\beta$ extreme value, so that a model with a slightly higher $\beta$ value would no longer collapse.