Effects of initial density profiles on massive star cluster formation in giant molecular clouds

@article{Chen2021EffectsOI,
  title={Effects of initial density profiles on massive star cluster formation in giant molecular clouds},
  author={Ying-Tung Chen and Hui Li and Mark Vogelsberger},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2021},
  volume={502},
  pages={6157-6169}
}
We perform a suite of hydrodynamic simulations to investigate how initial density profiles of giant molecular clouds (GMCs) affect their subsequent evolution. We find that the star formation duration and integrated star formation efficiency of the whole clouds are not sensitive to the choice of different profiles but are mainly controlled by the interplay between gravitational collapse and stellar feedback. Despite this similarity, GMCs with different profiles show dramatically different modes… Expand

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References

SHOWING 1-10 OF 101 REFERENCES
Physical Processes in Star Formation
Star formation is a complex multi-scale phenomenon that is of significant importance for astrophysics in general. Stars and star formation are key pillars in observational astronomy from local starExpand
A parallel non-uniform fast Fourier transform library based on an "exponential of semicircle" kernel
TLDR
FINUFFT is presented, an efficient parallel library for type 1 (nonuiform to uniform), type 2 (uniform to nonuniform), or type 3 (non uniform toNonuniform) transforms, in dimensions 1, 2, or 3, which uses minimal RAM, requires no precomputation or plan steps, and has a simple interface to several languages. Expand
Star Formation in Self-Gravitating Turbulent Fluids
We present a model of star formation in self-gravitating turbulent gas. We treat the turbulent velocity $v_T$ as a dynamical variable, and assume that it is adiabatically heated by the collapse. TheExpand
ALMA survey of massive cluster progenitors from ATLASGAL. Limited fragmentation at the early evolutionary stage of massive clumps
The early evolution of massive cluster progenitors is poorly understood. We investigate the fragmentation properties from 0.3 pc to 0.06 pc scales of a homogenous sample of infrared-quiet massiveExpand
Infall through the evolution of high-mass star-forming clumps
With the GREAT receiver at the Stratospheric Observatory for Infrared Astronomy (SOFIA), nine massive molecular clumps have been observed in the ammonia $3_{2+}- 2_{2-}$ line at 1.8~THz in a searchExpand
Understanding star formation in molecular clouds - I. Effects of line-of-sight contamination on the column density structure
Column-density maps of molecular clouds are one of the most important observables in the context of molecular cloud- and star-formation (SF) studies. With the Herschel satellite it is now possible toExpand
FRAGMENTATION OF MASSIVE DENSE CORES DOWN TO 1000 AU: RELATION BETWEEN FRAGMENTATION AND DENSITY STRUCTURE ∗
In order to shed light on the main physical processes controlling fragmentation of massive dense cores, we present a uniform study of the density structure of 19 massive dense cores, selected to beExpand
E pur si muove: Galilean-invariant cosmological hydrodynamical simulations on a moving mesh
Hydrodynamic cosmological simulations at present usually employ either the Lagrangian smoothed particle hydrodynamics (SPH) technique or Eulerian hydrodynamics on a Cartesian mesh with (optional)Expand
Density profiles in molecular cloud cores associated with high-mass star-forming regions
Radial density profiles for the sample of dense cores associated with high-mass star-forming regions from southern hemisphere have been derived using the data of observations in continuum at 250 GHz.Expand
The Physical Conditions for Massive Star Formation: Dust Continuum Maps and Modeling
Fifty-one dense cores associated with water masers were mapped at 350 μm. These cores are very luminous, 103 < Lbol/L☉ < 106, indicative of the formation of massive stars. Dust continuum contourExpand
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4
5
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