Spectral Properties of Compressible Magnetohydrodynamic Turbulence from Numerical Simulations

Details Spectral Properties of Compressible Magnetohydrodynamic Turbulence from Numerical Simulations Spectral Properties of Compressible Magnetohydrodynamic Turbulence from Numerical Simulations

2003-03-05

arxiv.org/abs/astro-ph/0303103v1

Astrophys.J. 590 (2003) 858-873

Astronomy and Astrophysics

Astrophysics

22 pages, 11 figures; Ap.J., accepted

Scientific paper

10.1086/375021

We analyze the spectral properties of driven, supersonic compressible magnetohydrodynamic (MHD) turbulence obtained via high-resolution numerical experiments, for application to understanding the dynamics of giant molecular clouds. Via angle-averaged power spectra, we characterize the transfer of energy from the intermediate, driving scales down to smaller dissipative scales, and also present evidence for inverse cascades that achieve modal-equipartition levels on larger spatial scales. Investigating compressive versus shear modes separately, we evaluate their relative total power, and find that as the magnetic field strength decreases, (1) the shear fraction of the total kinetic power decreases, and (2) slopes of power-law fits over the inertial range steepen. To relate to previous work on incompressible MHD turbulence, we present qualitative and quantitative measures of the scale-dependent spectral anisotropy arising from the shear-Alfv\'{e}n cascade, and show how these vary with changing mean magnetic field strength. Finally, we propose a method for using anisotropy in velocity centroid maps as a diagnostic of the mean magnetic field strength in observed cloud cores.

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