The density distribution and physical origins of intermittency in supersonic, highly magnetized turbulence with diverse modes of driving

Beattie, James R.; Mocz, Philip; Federrath, Christoph; Klessen, Ralf S.

doi:10.1093/mnras/stac3005

Title: The density distribution and physical origins of intermittency in supersonic, highly magnetized turbulence with diverse modes of driving

Journal Article · Sat Oct 22 00:00:00 EDT 2022 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stac3005· OSTI ID:1959545

^[1];

^[2]; Federrath, Christoph ^[3];

^[4]

Australian National Univ., Canberra, ACT (Australia); Univ. of California, Santa Cruz, CA (United States)
Princeton Univ., NJ (United States); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Australian National Univ., Canberra, ACT (Australia); Australian Research Council Center of Excellence in All Sky Astrophysics (ASTRO3D), Canberra, ACT (Australia)
Heidelberg Univ. (Germany). Institut fuer Theoretische Physik

The probability density function (PDF) of the logarithmic density contrast, s = ln (ρ/ρ₀), with gas density ρ and mean density ρ₀, for hydrodynamical supersonic turbulence is well known to have significant non-Gaussian (intermittent) features that monotonically increase with the turbulent Mach number, M. By studying the mass- and volume-weighted s-PDF for an ensemble of 36 sub-to-trans-Alfvenic 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 magnetized plasma for M≲4. However, for M≳4, the non-Gaussian signatures disappear, leaving approximately Gaussian s-statistics – exactly the opposite of hydrodynamical turbulence in the high-M limit. We also find that the non-Gaussian components of the PDF increase monotonically with more compressive driving modes. To understand the M≲4 non-Gaussian features, we use one-dimensional pencil beams to explore the dynamics along and across the large-scale magnetic field, B₀. Here 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 B₀. We discuss the Gaussianization of the M≳4 s-fields through the lens of two phenomenologies: the self-similarity of the s-field and homogenization of the dynamical time-scales between the over- and underdense regions in the compressible gas.

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Research Organization:: Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)

Sponsoring Organization:: USDOE National Nuclear Security Administration (NNSA); National Aeronautics and Space Administration (NASA); European Research Council (ERC); Gauss Centre for Supercomputing

Grant/Contract Number:: AC52-07NA27344; PF7-180164; 855130; pr32lo; pr48pi; pr74nu; pn73f

OSTI ID:: 1959545

Report Number(s):: LLNL-JRNL-826867; 1041342; TRN: US2312884

Journal Information:: Monthly Notices of the Royal Astronomical Society, Vol. 517, Issue 4; ISSN 0035-8711

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United States

Language:: English

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