Taking off the edge -- simultaneous filament and end core formation

Abstract

Simulations of idealised star-forming filaments of finite length typically show core growth which is dominated by two cores forming at its respective end. The end cores form due to a strong increasing acceleration at the filament ends which leads to a sweep-up of material during the filament collapse along its axis. As this growth mode is typically faster than any other core formation mode in a filament, the end cores usually dominate in mass and density compared to other cores forming inside a filament. However, observations of star-forming filaments do not show this prevalence of cores at the filament ends. We explore a possible mechanism to slow the growth of the end cores using numerical simulations of simultaneous filament and embedded core formation, in our case a radially accreting filament forming in a finite converging flow. While such a setup still leads to end cores, they soon begin to move inwards and a density gradient is formed outside of the cores by the continued accumulation of material. As a result, the outermost cores are not longer located at the exact ends of the filament and the density gradient softens the inward gravitational acceleration of the cores. Therefore, the two end cores do not grow as fast as expected and thus do not dominate over other core formation modes in the filament.

References in corpus (14)

• On the nature of star-forming filaments: I. Filament morphologies
• On the Structure of the Orion A Cloud and the Formation of the Orion Nebula Cluster
• The dynamical properties of dense filaments in the infrared dark cloud G035.39-00.33
• Aspect Ratio Dependence of the Free-Fall Time for Non-Spherical Symmetries
• Investigating the Global Collapse of Filaments Using Smoothed Particle Hydrodynamics
• Self-gravitating Filament Formation from Shocked Flows: Velocity Gradients across Filaments
• Observational signatures of end-dominated collapse in the S242 filamentary structure
• The JCMT Gould Belt Survey: A First Look at IC 5146
• Dense gas formation in the Musca filament due to the dissipation of a supersonic converging flow
• Edge collapse and subsequent longitudinal accretion in Filament S242
• Star-forming sites IC 446 and IC 447: an outcome of end-dominated collapse of Monoceros R1 filament
• Accretion driven turbulence in filaments II: Effects of self-gravity
• Merging Filaments I: A race against collapse
• Star Formation in a Strongly Magnetized Cloud

Cited by in corpus (3)

• Filament collapse: a two phase process
• Probing the Global Dust Properties and Cluster Formation Potential of the Giant Molecular Cloud G148.24+00.41
• Filament fragmentation: Density gradients suppress end dominated collapse