The contribution of binary star formation via core-fragmentation on protostellar multiplicity

TL;DR

This study investigates how core fragmentation influences the formation of close binary star systems, demonstrating that it can produce many such binaries without disc fragmentation, and highlights the environmental impact on multiplicity.

Contribution

It provides simulation-based evidence that core fragmentation significantly contributes to close binary formation, challenging the notion that disc fragmentation is necessary.

Findings

Core fragmentation accounts for ~60% of multiple systems.

Close binaries (20-100AU) can form via core fragmentation or dynamical capture.

Bimodal multiplicity distribution can be replicated in simulations.

Abstract

Observations of young multiple star systems find a bimodal distribution in companion frequency and separation. The origin of these peaks has often been attributed to binary formation via core and disc fragmentation. However, theory and simulations suggest that young stellar systems that form via core fragmentation undergo significant orbital evolution. We investigate the influence of the environment on the formation and orbital evolution of multiple star systems, and how core fragmentation contributes to the formation of close (20-100AU) binaries. We use multiple simulations of star formation in giant molecular clouds and compare them to the multiplicity statistics of the Perseus star-forming region. Simulations were run with the adaptive mesh refinement code RAMSES with sufficient resolution to resolve core fragmentation beyond 400AU and dynamical evolution down to 16.6AU, but without the possibility of resolving disc fragmentation. The evolution of the resulting stellar systems was followed over millions of years. We find that star formation in lower gas density environments is more clustered; however, despite this, the fractions of systems that form via dynamical capture and core fragmentation are broadly consistent at ~40\% and ~60\%, respectively. We then compared the simulation with the conditions most similar to the Perseus star-forming region to determine whether the observed bimodal distribution can be replicated. We find that it can be replicated, but it is sensitive to the evolutionary state of the simulation. Our results indicate that a significant number of low-mass close binaries with separations from 20-100AU can be produced via core fragmentation or dynamical capture due to efficient inspiral, without the need for a further contribution from disc fragmentation.