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Helical and nonhelical magnetohydrodynamic (MHD) turbulence simulations reveal minimal inverse energy transfer, influenced by Prandtl number. Decaying laws depend on Prandtl and Reynolds numbers, not scale separation.

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Area of Science:

  • Physics
  • Astrophysics
  • Fluid Dynamics

Background:

  • Helical magnetohydrodynamic (MHD) turbulence is known for inverse energy transfer due to magnetic helicity conservation.
  • Recent studies suggest inverse energy transfer may occur in nonhelical MHD flows.

Purpose of the Study:

  • Investigate inverse energy transfer in both helical and nonhelical MHD flows.
  • Analyze the decaying laws of MHD turbulence across various parameters.
  • Compare simulation results with existing literature.

Main Methods:

  • Direct numerical simulations (DNS) of MHD turbulence.
  • Extensive parameter study including Prandtl number (Pm) and Reynolds number (Re).
  • Analysis of energy transfer and decay rates.

Main Results:

  • A small inverse energy transfer was observed, increasing with the Prandtl number.
  • Decaying laws (E~t^{-p}) were found to be independent of scale separation, depending only on Pm and Re.
  • In helical cases, decay exponent p_b showed a dependence on Re (p_b ≈ 0.6 + 14/Re).

Conclusions:

  • The Prandtl number plays a role in inverse energy transfer in MHD turbulence.
  • Findings have implications for understanding cosmic magnetic field evolution.
  • Decay characteristics are primarily governed by fluid properties (Pm, Re) rather than flow geometry.