Necessary conditions for the formation of filaments and star clusters in the cold neutral medium

Abstract

Star formation takes place in filamentary molecular clouds which arise by physical processes that take place in the cold, neutral medium (CNM). We address the necessary conditions for this diffuse ($n\approx 30$ cm${}^{-3}$), cold (T $\approx$ 60 K), magnetized gas undergoing shock waves and supersonic turbulence, to produce filamentary structures capable of fragmenting into cluster forming regions. Using RAMSES and a magnetized CNM environment as our initial conditions, we simulate a 0.5 kpc turbulent box to model a uniform gas with magnetic field strength of 7 $\mu G$, varying the 3D velocity dispersion via decaying turbulence. We use a surface density of $320M_{\odot }p{c}^{-2}$, representative of the inner 4.0 kpc CMZ of the Milky Way and typical luminous galaxies. Filamentary molecular clouds are formed dynamically via shocks within a narrow range of velocity dispersions in the CNM of 5 - 10 km/s with a preferred value at 8 km/s. Cluster sink particles appear in filaments which exceed their critical line mass, occurring optimally for velocity dispersions of 8 km/s. Tracking the evolution of magnetic fields, we find that they lead to double the dense star forming gas than in purely hydro runs. Perpendicular orientations between magnetic field and filaments can increase the accretion rates onto filaments and hence their line masses. Because magnetic fields help support gas, MHD runs result in average temperatures an order of magnitude higher than unmagnetized counterparts. Finally, we find magnetic fields delay the onset of cluster formation by $\propto 0.4$ Myr.

25 pages, 20 figures, to be published in Monthly Notices of the Royal Astronomical Society accepted December 22 2023

References in corpus (46)

• Filamentary structure of star-forming complexes
• Modeling Collapse and Accretion in Turbulent Gas Clouds: Implementation and Comparison of Sink Particles in AMR and SPH
• Grackle: a Chemistry and Cooling Library for Astrophysics
• CO Isotopologues in the Perseus Molecular Cloud Complex: the X-Factor and Regional Variations
• Numerical simulations of compressively driven interstellar turbulence: I. Isothermal gas
• Herschel-Planck dust optical-depth and column-density maps: I. Method description and results for Orion
• Dependence of Interstellar Turbulent Pressure on Supernova Rate
• The dynamics and outcome of star formation with jets, radiation, winds, and supernovae in concert
• Towards a more realistic sink particle algorithm for the RAMSES code
• Unfolding the Laws of Star Formation: The Density Distribution of Molecular Clouds
• Star cluster formation in cosmological simulations. I. Properties of young clusters
• The PHANGS-HST Survey: Physics at High Angular resolution in Nearby GalaxieS with the Hubble Space Telescope
• Molecular Cloud Populations in the Context of Their Host Galaxy Environments: A Multiwavelength Perspective
• SILCC VI -- Multi-phase ISM structure, stellar clustering, and outflows with supernovae, stellar winds, ionising radiation and cosmic rays
• Magnetically Dominated Strands of Cold Hydrogen in the Riegel-Crutcher Cloud
• The Massive Star-forming Regions Omnibus X-ray Catalog
• Efficient early stellar feedback can suppress galactic outflows by reducing supernova clustering
• On the Three-Dimensional Structure of Local Molecular Clouds
• Magnetized filamentary gas flows feeding the young embedded cluster in Serpens South
• A model for the formation of stellar associations and clusters from giant molecular clouds
• Herschel's view of the large-scale structure in the Chamaeleon dark clouds
• PHANGS-JWST First Results: A statistical view on bubble evolution in NGC628
• Introducing EMP-Pathfinder: modelling the simultaneous formation and evolution of stellar clusters in their host galaxies
• The role of galactic dynamics in shaping the physical properties of giant molecular clouds in Milky Way-like galaxies
• The Role of Turbulence and Magnetic Fields in Simulated Filamentary Structure
• 3D chemical structure of diffuse turbulent ISM. I. Statistics of the HI-to-H${}_2$ transition
• B-fields in Star-Forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main
• Quantifying the energetics of molecular superbubbles in PHANGS galaxies
• Sub-parsec resolution cosmological simulations of star-forming clumps at high redshift with feedback of individual stars
• The Galactic dynamics revealed by the filamentary structure in atomic hydrogen emission
• Cloud formation in the atomic and molecular phase: HI self absorption (HISA) towards a Giant Molecular Filament
• The 3-D Kinematics of the Orion Nebula Cluster: NIRSPEC-AO Radial Velocities of the Core Population
• Orion A's complete 3D magnetic field morphology
• The core and stellar mass functions in massive collapsing filaments
• Large-scale turbulent driving regulates star formation in high-redshift gas-rich galaxies
• PHANGS: Constraining Star Formation Timescales Using the Spatial Correlations of Star Clusters and Giant Molecular Clouds
• Embedded Young Massive Star Clusters in the Antennae Merger
• A two-step gravitational cascade for the fragmentation of self-gravitating discs
• Molecular clumps photoevaporation in ionized regions
• The SATIN project I: Turbulent multi-phase ISM in Milky Way simulations with SNe feedback from stellar clusters
• Testing Feedback from Star Clusters in Simulations of the Milky Way Formation
• Large-scale turbulent driving regulates star formation in high-redshift gas-rich galaxies II: Influence of the magnetic field and the turbulent compressive fraction
• Extreme giant molecular clouds in the luminous infrared galaxy NGC 3256
• A nearly constant CN/HCN line ratio in nearby galaxies: CN as a new tracer of dense gas
• Physical Properties and Scaling Relations of Molecular Clouds: the Impact of Star Formation
• Impact of Radiation Feedback on the Formation of Globular Cluster Candidates during Cloud-Cloud Collisions

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