Competitive accretion in embedded stellar cluster

Abstract

We investigate the physics of gas accretion in young stellar clusters. Accretion in clusters is a dynamic phenomenon as both the stars and the gas respond to the same gravitational potential. Accretion rates are highly non-uniform with stars nearer the centre of the cluster, where gas densities are higher, accreting more than others. This competitive accretion naturally results in both initial mass segregation and a spectrum of stellar masses. Accretion in gas-dominated clusters is well modelled using a tidal-lobe radius instead of the commonly used Bondi-Hoyle accretion radius. This works as both the stellar and gas velocities are under the influence of the same gravitational potential and are thus comparable. The low relative velocity that results means that the tidal radius is smaller than the Bondi-Hoyle radius in these systems. In contrast, when the stars dominate the potential and are virialised, the Bondi-Hoyle radius is smaller than the tidal radius and thus Bondi-Hoyle accretion is a better fit to the accretion rates.

11 pages, 11 figures, MNRAS in press

Cited by in corpus (385)

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• The Luminosity Problem: Testing Theories of Star Formation
• Gas and star kinematics in cloud-cloud collisions
• Star-forming environments in smoothed particle magnetohydrodynamics simulations I: Clump extraction and properties
• Modeling High-Mass Star Formation and Ultracompact HII Regions
• Formation of low-mass stars and brown dwarfs
• Synthetic ngVLA line observations of a massive star-forming cloud
• The outer orbit of the high-mass stellar triple system Herschel 36 determined with the VLTI
• On the evolution of irradiated turbulent clouds: A comparative study between modes of triggered star-formation
• The molecular environment of the Galactic star forming region G19.61-0.23
• Competitive Accretion and the IMF
• Isolating the pre-main sequence in Collinder34, NGC3293, NGC3766 and NG6231
• Simulations of the IMF in Clusters
• Clustered Star Formation: A Review
• The Deuteration Clock for Massive Starless Cores
• Accretion-caused deceleration of a gravitationally powerful compact stellar object moving within a dense Fermi gas
• ATLASGAL-selected high-mass clumps in the inner Galaxy: XI. Morphology and kinematics of warm inner envelopes
• Deuterium fractionation of the starless core L 1498
• A framework for modeling the evolution of young stellar objects
• Fire from Ice - Massive Star Birth from Infrared Dark Clouds
• Stars Form By Gravitational Collapse, Not Competitive Accretion
• Empirical formulae to describe some physical properties of small groups of protogalaxies with multiplicity
• Gamma Analytical Modeling Evolution (GAME) I: The physical implications of deriving the stellar mass functions from z=0 to z=8
• Gauging the Impact of Cosmic Ray Feedback on the Stellar Initial Mass Function
• Properties of Contracting Massive Protostellar Cores
• Star Formation
• Synthetic observations using POLARIS: an application to simulations of massive prestellar cores
• The Carina High-Contrast Imaging Project for massive Stars (CHIPS) I. Methodology and proof of concept on QZ Car ($\equiv$ HD93206)
• Unraveling the Spectral Energy Distributions of Clustered YSOs
• From Interstellar Clouds to Stars
• The Plaskett Lecture: Star Formation in the Perseus Molecular Cloud
• Open clusters: their kinematics and metellicities