As a Matter of Tension: Kinetic Energy Spectra in MHD Turbulence

@article{Grete2020AsAM,
  title={As a Matter of Tension: Kinetic Energy Spectra in MHD Turbulence},
  author={Philipp Grete and Brian W. O’Shea and Kris Beckwith},
  journal={The Astrophysical Journal},
  year={2020},
  volume={909}
}
While magnetized turbulence is ubiquitous in many astrophysical and terrestrial systems, our understanding of even the simplest physical description of this phenomena, ideal magnetohydrodynamic (MHD) turbulence, remains substantially incomplete. In this work, we highlight the shortcomings of existing theoretical and phenomenological descriptions of MHD turbulence that focus on the joint (kinetic and magnetic) energy fluxes and spectra by demonstrating that treating these quantities separately… 
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References

SHOWING 1-10 OF 86 REFERENCES
The Intermittency of ISM Turbulence: What Do the Observations Tell Us?
The interstellar medium is highly turbulent, but this medium, a partially ionized plasma, is also multi-phase, compressible and magnetized, hence the complexity of its turbulence extends beyond
Turbulence in the Intracluster Medium
We review our knowledge about turbulence in the intracluster medium, a very hot, dilute plasma that permeates clusters of galaxies. A thorough understanding of turbulence in the intracluster medium
Interstellar MHD Turbulence and Star Formation
This chapter reviews the nature of turbulence in the Galactic interstellar medium (ISM) and its connections to the star formation (SF) process. The ISM is turbulent, magnetized, self-gravitating, and
Cosmic Rays in Galaxy Clusters and Their Interaction with Magnetic Fields
Cosmic rays can be accelerated in galaxy clusters by different mechanisms and remain confined in the cluster volume accumulating for cosmological times. This component is expected to generate
Implicit Large Eddy Simulation: Computing Turbulent Fluid Dynamics
Introduction Fernando Grinstein, Len Margolin and William Rider Part I. Motivation: 1. Historical introduction Jay Boris 2. ILES for turbulent flows: a rationale Fernando Grinstein, Len Margolin and
Interstellar MHD Turbulence and Star
  • PhPl,
  • 2011
RvMP, 70, 1 Beresnyak, A
  • PhRvL,
  • 2010
K-Athena: A Performance Portable Structured Grid Finite Volume Magnetohydrodynamics Code
TLDR
This work combines an existing magnetohydrodynamics CPU code with a performance portable on-node parallel programming paradigm into K-Athena to allow efficient simulations on multiple architectures using a single codebase and presents profiling and scaling results for different platforms.
  • Webplotdigitizer: Version 4.3.
  • 2020
Impact of Magnetorotational Instability on Grain Growth in Protoplanetary Disks. I. Relevant Turbulence Properties
Turbulence in the protoplanetary disks induces collisions between dust grains, and thus facilitates grain growth. We investigate the two fundamental assumptions of the turbulence in obtaining grain
...
1
2
3
4
5
...