Driven Multifluid MHD Molecular Cloud Turbulence

Abstract

It is believed that turbulence may have a significant impact on star formation and the dynamics and evolution of the molecular clouds in which this occurs. It is also known that non-ideal magnetohydrodynamic effects influence the nature of this turbulence. We present the results of a numerical study of 4-fluid MHD turbulence in which the dynamics of electrons, ions, charged dust grains and neutrals and their interactions are followed. The parameters describing the fluid being simulated are based directly on observations of molecular clouds. We find that the velocity and magnetic field power spectra are strongly influenced by multifluid effects on length-scales at least as large as 0.05 pc. The PDFs of the various species in the system are all found to be close to log-normal, with charged species having a slightly less platykurtic (flattened) distribution than the neutrals. We find that the introduction of multifluid effects does not significantly alter the structure functions of the centroid velocity increment.

15 pages, 14 figures, 5 tables. Accepted for publication in MNRAS

References in corpus (8)

• The Density Probability Distribution in Compressible Isothermal Turbulence: Solenoidal versus Compressive Forcing
• Simulating the formation of molecular clouds. II. Rapid formation from turbulent initial conditions
• Density Probability Distribution Functions in Supersonic Hydrodynamic and MHD Turbulence
• Probing the Turbulence Dissipation Range and Magnetic Field Strengths in Molecular Clouds
• Sub-Alfvenic Non-Ideal MHD Turbulence Simulations with Ambipolar Diffusion: I. Turbulence Statistics
• A three-dimensional numerical method for modelling weakly ionized plasmas
• Three-dimensional Simulation of Magnetized Cloud Fragmentation Induced by Nonlinear Flows and Ambipolar Diffusion
• Dissipative structures of diffuse molecular gas III -- Small-scale intermittency of intense velocity-shears

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• Some Stars are Totally Metal: A New Mechanism Driving Dust Across Star-Forming Clouds, and Consequences for Planets, Stars, and Galaxies
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• Small-scale clustering of nano-dust grains in supersonic turbulence
• A JWST Preview: Adaptive-Optics Images of H${}_2$, Br-$\gamma$, and K-continuum in Carina's Western Wall
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