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Mueller, Wolf-Christian; Grappin, Roland (2005)
Languages: English
Types: Preprint
Subjects: Physics - Fluid Dynamics, Physics - Plasma Physics

Classified by OpenAIRE into

arxiv: Physics::Space Physics
Spectral direct numerical simulations of incompressible MHD turbulence at a resolution of up to $1024^3$ collocation points are presented for a statistically isotropic system as well as for a setup with an imposed strong mean magnetic field. The spectra of residual energy, $E_k^\mathrm{R}=|E_k^\mathrm{M}-E_k^\mathrm{K}|$, and total energy, $E_k=E^\mathrm{K}_k+E^\mathrm{M}_k$, are observed to scale self-similarly in the inertial range as $E_k^\mathrm{R}\sim k^{-7/3}$, $E_k\sim k^{-5/3}$ (isotropic case) and $E^\mathrm{R}_{k_\perp}\sim k_\perp^{-2}$, $E_{k_\perp}\sim k_\perp^{-3/2}$ (anisotropic case, perpendicular to the mean field direction). A model of dynamic equilibrium between kinetic and magnetic energy, based on the corresponding evolution equations of the eddy-damped quasi-normal Markovian (EDQNM) closure approximation, explains the findings. The assumed interplay of turbulent dynamo and Alfv\'en effect yields $E_k^\mathrm{R}\sim k E^2_k$ which is confirmed by the simulations.
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    • [1] S. Ortolani and D. D. Schnack, Magnetohydrodynamics of Plasma Relaxation (World Scientific, Singapore, 1993).
    • [2] Y. B. Zeldovich, A. A. Ruzmaikin, and D. D. Sokoloff, Magnetic Fields In Astrophysics (Gordon and Breach Science Publishers, New York, 1983).
    • [3] D. Biskamp, Magnetohydrodynamic Turbulence (Cambridge University Press, Cambridge, 2003).
    • [4] A. N. Kolmogorov, Proceedings of the Royal Society A 434, 9 (1991), [Dokl. Akad. Nauk SSSR, 30(4), 1941].
    • [5] P. S. Iroshnikov, Soviet Astronomy 7, 566 (1964), [Astron. Zh., 40:742, 1963].
    • [6] R. H. Kraichnan, Physics of Fluids 8, 1385 (1965).
    • [7] P. Goldreich and S. Sridhar, Astrophysical Journal 485, 680 (1997).
    • [8] S. Sridhar and P. Goldreich, Astrophysical Journal 432, 612 (1994).
    • [9] W.-C. Mu¨ller and D. Biskamp, in Turbulence and Magnetic Fields in Astrophysics, edited by E. Falgarone and T. Passot (Springer Berlin, 2002), vol. 614 of Lecture Notes in Physics, pp. 3-27.
    • [10] R. Grappin, A. Pouquet, and J. L´eorat, Astronomy and Astrophysics 126, 51 (1983).
    • [11] A. Vincent and M. Meneguzzi, Journal of Fluid Mechanics 225, 1 (1991).
    • [12] D. Biskamp and W.-C. Mu¨ller, Physical Review Letters 83, 2195 (1999).
    • [13] W.-C. Mu¨ller and D. Biskamp, Physical Review Letters 84, 475 (2000).
    • [14] N. E. L. Haugen, A. Brandenburg, and W. Dobler, Physical Review E 70, 016308 (2004).
    • [15] R. J. Leamon, C. W. Smith, N. F. Ness, W. H. Matthaeus, and H. K. Wong, Journal of Geophysical Research 103, 4775 (1998).
    • [16] M. L. Goldstein and D. A. Roberts, Physics of Plasmas 6, 4154 (1999).
    • [17] Y. Kaneda, T. Ishihara, M. Yokokawa, K. Itakura, and A. Uno, Physics of Fluids 15, L21 (2003).
    • [18] W.-C. Mu¨ller, D. Biskamp, and R. Grappin, Physical Review E 67, 066302 (2003).
    • [19] R. Grappin, Physics of Fluids 29, 2433 (1986).
    • [20] J. V. Shebalin, W. H. Matthaeus, and D. Montgomery, Journal of Plasma Physics 29, 525 (1983).
    • [21] R. M. Kinney and J. C. McWilliams, Physical Review E 57, 7111 (1998).
    • [22] S. Oughton, W. H. Matthaeus, and S. Ghosh, Physics of Plasmas 5, 4235 (1998).
    • [23] J. Cho, A. Lazarian, and E. T. Vishniac, Astrophysical Journal 564, 291 (2002).
    • [24] J. Cho and E. T. Vishniac, Astrophysical Journal 539, 273 (2000).
    • [25] J. Maron and P. Goldreich, Astrophysical Journal 554, 1175 (2001).
    • [26] S. A. Orszag, Journal of Fluid Mechanics 41, 363 (1970).
    • [27] A. Pouquet, U. Frisch, and J. L´eorat, Journal of Fluid Mechanics 77, 321 (1976).
    • [28] R. Grappin, U. Frisch, J. L´eorat und A. Pouquet, Astronomy and Astrophysics 105, 6 (1982).
    • [29] M. Lesieur, Turbulence in Fluids (Kluwer Academic Publishers, Dordrecht, 1997).
    • [30] J. Heyvaerts and E. R. Priest, Astronomy & Astrophysics 117, 220 (1983).
    • [31] D. Biskamp, Chaos, Solitons & Fractals 5, 1779 (1995).
    • [32] The other definition of EkR involving the modulus op-
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