Context. Direct numerical simulations of plasmas have shown that the dynamo effect is efficient even at low Prandtl numbers, i.e., the critical magnetic Reynolds number Rmc that is necessary for a dynamo to be efficient becomes smaller than the hydrodynamic Reynolds number Re when Re → ∞.
Aims: We test the conjecture that Rmc tends to a finite value when Re → ∞, and we study the behavior of the dynamo growth factor γ at very low and high magnetic Prandtl numbers.
Methods: We use local and nonlocal shell models of magnetohydrodynamic (MHD) turbulence with parameters covering a much wider range of Reynolds numbers than direct numerical simulations, that is of astrophysical relevance.
Results: We confirm that Rmc tends to a finite value when Re → ∞. As Rm → ∞, the limit to the dynamo growth factor γ in the kinematic regime follows Reβ, and, similarly, the limit for Re → ∞ of γ behaves like Rmβ', with β ≈ β' ≈ 0.4.
Conclusions: Our comparison with a phenomenology based on an intermittent small-scale turbulent dynamo, together with the differences between the growth rates in the different local and nonlocal models, indicate that nonlocal terms contribute weakly to the dynamo effect.
Astronomy and Astrophysics
- Pub Date:
- October 2011
- magnetohydrodynamics (MHD);
- Physics - Plasma Physics;
- Astrophysics - Solar and Stellar Astrophysics
- 5 pages, 6 figures