Star Cluster Formation in Clouds with Externally Driven Turbulence
arXiv:2208.05474 · doi:10.1093/mnras/stac2295
Abstract
Star clusters are known to be formed in turbulent molecular clouds. How turbulence is driven in molecular clouds and what effect this has on star formation is still unclear. We compare a simulation setup with turbulent driving everywhere in a periodic box with a setup where turbulence is only driven around the outside of the box. We analyse the resulting gas distribution, kinematics, and the population of stars that are formed from the cloud. Both setups successfully produce a turbulent velocity field with a power law structure function, the externally driven cloud has a more central, monolithic, clump, while the fully driven cloud has many smaller, more dispersed, clumps. The star formation follows the cloud morphology producing large clusters, with high star forming efficiency in the externally driven simulations and sparse individual star formation with much lower star formation efficiency in the fully driven case. We conclude that the externally driven method, which resembles a Global Hierarchical Collapse (GHC) scenario, produces star clusters that more closely match with observations.
arXiv comment8 pages, 6 figures, accepted by MNRAS
References in corpus (49)
- Embedded Clusters in Molecular Clouds
- Interstellar Turbulence I: Observations and Processes
- Modelling Accretion in Protobinary Systems
- The Statistics of Supersonic Isothermal Turbulence
- Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics
- Global Hierarchical Collapse In Molecular Clouds. Towards a Comprehensive Scenario
- A Unified Model for Galactic Discs: Star Formation, Turbulence Driving, and Mass Transport
- Inefficient star formation through turbulence, magnetic fields and feedback
- Feedback-regulated star formation in molecular clouds and galactic discs
- On the universality of interstellar filaments: theory meets simulations and observations
- Supernova Driving. I. The Origin of Molecular Cloud Turbulence
- Importance of the Initial Conditions for Star Formation - I. Cloud Evolution and Morphology
- Two regimes of Turbulent Fragmentation and the stellar IMF from Primordial to Present Day Star Formation
- When Feedback Fails: The Scaling and Saturation of Star Formation Efficiency
- Is Turbulence in the Interstellar Medium Driven by Feedback or Gravity? An Observational Test
- Collapse of a molecular cloud core to stellar densities: stellar core and outflow formation in radiation magnetohydrodynamics simulations
- SILCC-Zoom: The dynamical and chemical evolution of molecular clouds
- The impact of stellar feedback on the structure, size and morphology of galaxies in Milky Way size dark matter haloes
- Hierarchical Cluster Assembly in Globally Collapsing Clouds
- Driven and Decaying Turbulence Simulations of Low-Mass Star Formation: From Clumps to Cores to Protostars
- Moving mesh simulations of star forming cores in magneto-gravo-turbulence
- Supernova Driving. IV. The Star Formation Rate of Molecular Clouds
- STARFORGE: The effects of protostellar outflows on the IMF
- Mass Transport and Turbulence in Gravitationally Unstable Disk Galaxies II: The Effects of Star Formation Feedback
- Scaling Relations of Compressible MHD Turbulence
- The structure and statistics of interstellar turbulence
- What can simulated molecular clouds tell us about real molecular clouds?
- Stellar mass spectrum within massive collapsing clumps II. Thermodynamics and tidal forces of the first Larson core
- The Self-gravitating Gas Fraction and The Critical Density for Star Formation
- Stellar mass spectrum within massive collapsing clumps I. Influence of the initial conditions
- An Evolutionary Model for Collapsing Molecular Clouds and Their Star Formation Activity. II. Mass Dependence of the Star Formation Rate
- Is molecular cloud turbulence driven by external supernova explosions?
- The effect of photoionising feedback on the shaping of hierarchically-forming stellar clusters
- The effect of the virial state of molecular clouds on the influence of feedback from massive stars
- The IMF as a function of supersonic turbulence
- The formation of young massive clusters by colliding flows
- How do different spiral arm models impact the ISM and GMC population?
- The role of collision speed, cloud density, and turbulence in the formation of young massive clusters via cloud-cloud collisions
- Stellar mass spectrum within massive collapsing clumps III. Effects of temperature and magnetic field
- The hierarchical fragmentation of filaments and the role of sub-filaments
- The Effects of Magnetic Fields and Outflow Feedback on the Shape and Evolution of the Density PDF in Turbulent Star-Forming Clouds
- The onset of large scale turbulence in the interstellar medium of spiral galaxies
- Testing the Turbulent Origin of the Stellar Initial Mass Function
- Probing the structure of a massive filament: ArTeMiS 350 and 450 micron mapping of the integral-shaped filament in Orion A
- How do velocity structure functions trace gas dynamics in simulated molecular clouds?
- Simultaneous evolution of the virial parameter and star formation rate in molecular clumps undergoing global hierarchical collapse
- The properties of clusters, and the orientation of magnetic fields relative to filaments, in magnetohydrodynamic simulations of colliding clouds
- Gravoturbulent Star Formation: Effects of the Equation of State on Stellar Masses
- Symmetry properties and widths of the filamentary structures in the Orion A giant molecular cloud