On the thermal sensitivity of binary formation in collapsing molecular clouds

TL;DR

This study uses numerical simulations to explore how initial temperature and perturbations influence binary star formation in collapsing molecular clouds, revealing high sensitivity to thermal conditions and density transition effects.

Contribution

It provides new insights into the thermal sensitivity of binary formation and the role of the isothermal-to-adiabatic transition in protostellar evolution.

Findings

Initial temperature variations significantly affect binary separation.

Higher perturbation amplitudes promote binary formation.

Critical density impacts disk structure and fragmentation.

Abstract

We report the results of a numerical study on the initial formation stages of low-mass protostellar binary systems. We determine the separation of protostellar binaries formed as a function of the initial thermal state by varying the initial temperature in a slightly modified version of the Burkert and Bodenheimer collapse test. We find that the outcome is highly sensitive to both the initial temperature of the cloud and the initial amplitude of azimuthal density perturbation A. For A=10 %, variations of only 1 unit Kelvin below 10 K lead to changes of up to 100 AU ( i.e. of order 30 %) in the instantaneous separation, whereas for this small A the initial temperatures above 10 K yield, instead of a binary, a single low-mass fragment that never reaches protostellar densities. Protostellar binaries, however, do emerge when the perturbation amplitude is increased from 10 % to 25 %. We also investigate the impact of the critical density which governs the transition from isothermal to adiabatic thermodynamic behaviour of the collapsing gas. We find that the critical density not only affects the overall structural evolution of the gas envelope, but also the size of the rotating disk structures formed during collapse as well as the number of protostellar fragments resulting from the final fragmentation of the disks. This mechanism can give rise to young protostellar objects constituting bound multiple stellar systems.