The density distribution and physical origins of intermittency in supersonic, highly magnetised turbulence with diverse modes of driving
The probability density function (PDF) of the logarithmic density contrast, \mbox{$s=\ln (\rho/\rho_0)$}, with gas density $\rho$ and mean density $\rho_0$, for hydrodynamical supersonic turbulence is well-known to have significant non-Gaussian (intermittent) features that monotonically increase wit...
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| Main Authors: | , , , |
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| Format: | Article (Journal) Chapter/Article |
| Language: | English |
| Published: |
15 Oct 2022
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| Edition: | Version V3 |
| In: |
Arxiv
Year: 2022, Pages: 1-32 |
| DOI: | 10.48550/arXiv.2109.10470 |
| Online Access: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.48550/arXiv.2109.10470 Verlag, lizenzpflichtig, Volltext: http://arxiv.org/abs/2109.10470 
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| Author Notes: | James R. Beattie, Philip Mocz, Christoph Federrath and Ralf S. Klessen |
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| 245 | 1 | 4 | |a The density distribution and physical origins of intermittency in supersonic, highly magnetised turbulence with diverse modes of driving |c James R. Beattie, Philip Mocz, Christoph Federrath and Ralf S. Klessen |
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| 520 | |a The probability density function (PDF) of the logarithmic density contrast, \mbox{$s=\ln (\rho/\rho_0)$}, with gas density $\rho$ and mean density $\rho_0$, for hydrodynamical supersonic turbulence is well-known to have significant non-Gaussian (intermittent) features that monotonically increase with the turbulent Mach number, $\mathcal{M}$. By studying the mass- and volume-weighted $s$-PDF for an ensemble of 36 sub-to-trans-Alf\'venic mean-field, supersonic, isothermal turbulence simulations with different modes of driving, relevant to molecular gas in the cool interstellar medium, we show that a more intricate picture emerges for the non-Gaussian nature of $s$. Using four independent measures of the non-Gaussian components, we find hydrodynamical-like structure in the highly magnetised plasma for $\mathcal{M} \lesssim 4$. However, for $\mathcal{M} \gtrsim 4$, the non-Gaussian signatures disappear, leaving approximately Gaussian $s$-statistics -- exactly the opposite of hydrodynamical turbulence in the high-$\mathcal{M}$ limit. We also find that the non-Gaussian components of the PDF increase monotonically as the turbulence evolves from solenoidally-driven to compressively-driven. To understand the $\mathcal{M} \lesssim 4$ non-Gaussian features we use one-dimensional (1D) pencil beams to explore the dynamics along and across the large-scale magnetic field, $\mathbf{B}_0$. We discuss kinetic, density and magnetic field fluctuations from the pencil beams, and identify physical sources of non-Gaussian components to the PDF as single, strong shocks coupled to fast magnetosonic compressions that form along $\mathbf{B}_0$ and create large, volume-poor under-densities. These under-densities contribute significantly to the skewness of the $s$-PDF. We confirm this result independently using 1D fluid shock simulations. We discuss the Gaussianisation of the $\mathcal{M} \gtrsim 4$... | ||
| 650 | 4 | |a Astrophysics - Astrophysics of Galaxies | |
| 650 | 4 | |a Physics - Fluid Dynamics | |
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| 700 | 1 | |a Federrath, Christoph |e VerfasserIn |0 (DE-588)141657138 |0 (DE-627)630407959 |0 (DE-576)324891598 |4 aut | |
| 700 | 1 | |a Klessen, Ralf S. |d 1968- |e VerfasserIn |0 (DE-588)120533820 |0 (DE-627)392381532 |0 (DE-576)178685399 |4 aut | |
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