Toward a Theory of Interstellar Turbulence. II. Strong Alfvenic Turbulence
Abstract
We continue to investigate the possibility that interstellar turbulence is caused by nonlinear interactions among shear Alfven waves. Here, we restrict attention to the symmetric case where the oppositely directed waves carry equal energy fluxes. This precludes application to the solar wind in which the outward flux significantly exceeds the ingoing one. All our detailed calculations are carried out for an incompressible magnetized fluid. In incompressible magnetohydrodynamics (MHD), nonlinear interactions only occur between oppositely direct waves. We present a theory for the strong turbulence of shear Alfven waves. It has the following main characteristics. (1) The inertialstage energy spectrum exhibits a critical balance between linear wave periods and nonlinear turnover timescales. (2) The 'eddies' are elongated in the direction of the field on small spatial scales; the parallel and perpendicular components of the wave vector, k_{z} and k(perpendicular) are related by k_{z} approximately equals k_{perpendicular to}^{2/3} L^{1/3}, where L is the outer scale of the turbulence. (3) The 'onedimensional' energy spectrum is proportional to k_{perpendicular}^{5/3}an anisotropic Kolmogorov energy spectrum. Shear Alfvenic turbulence mixes specific entropy as a passive contaminant. This gives rise to an electron density power spectrum whose form mimics the energy spectrum of the turbulence. Radio wave scattering by these electron density fluctuations produces anisotropic scatterbroadened images. Damping by ionneutral collisions restricts Alfvenic turbulence to highly ionized regions of the interstellar medium.
 Publication:

The Astrophysical Journal
 Pub Date:
 January 1995
 DOI:
 10.1086/175121
 Bibcode:
 1995ApJ...438..763G
 Keywords:

 Interstellar Space;
 Magnetic Fields;
 Magnetohydrodynamic Turbulence;
 Magnetohydrodynamic Waves;
 Electron Density (Concentration);
 Energy Spectra;
 Radio Waves;
 Variations;
 Wave Scattering;
 Astrophysics;
 ISM: GENERAL;
 MAGNETOHYDRODYNAMICS: MHD;
 TURBULENCE