On filament fragmentation and the impact of ambient environment on it

TL;DR

This study uses hydrodynamic simulations to investigate filament fragmentation in star formation, revealing how ambient pressure influences filament morphology, stability, and star formation efficiency.

Contribution

It demonstrates that external pressure significantly affects filament evolution and fragmentation, providing new insights into the environmental impact on star formation processes.

Findings

Fibres form naturally during filament formation.

Fragment morphology depends on external pressure.

Higher external pressure reduces star formation efficiency.

Abstract

Filaments are crucial intermediaries in the star formation process. Recent observations of filaments show that - \textbf{(i)} a number of them are non-singular entities, and rather a bundle of velocity coherent fibres, and \textbf{(ii)} while a majority of filaments spawn cores narrower than their natal filaments, some cores are broader. We explore these issues by developing hydrodynamic simulations of an initially sub-critical individual filament that is allowed to accrete gas from its neighbourhood and evolves under self-gravity. Results obtained here support the idea that fibres form naturally during the filament formation process. We further argue that the ambient environment, i.e., the magnitude of external pressure, and not the filament linemass alone, has bearing upon the morphology of its evolution. We observe that a filament is susceptible to the \emph{sausage}-type instability irrespective of the external pressure. The fragments, however, are pinched in a filament experiencing pressure comparable to that in the Solar neighbourhood ($\sim 10^{4}$ K cm$^{-3}$). By contrast, fragments are broad and spherical - having density profiles similar to that of a stable Bonnor - Ebert sphere - when the filament experiences a higher pressure, typically $\ge 10^{5}$ K cm$^{-3}$, but $\le 10^{6}$ K cm$^{-3}$). The filament tends to rupture at even higher external pressure ($\ge 10^{7}$ K cm$^{-3}$). These observations collectively mean that star formation is less efficient with increasing external pressure.