Intermittency and alignment in strong RMHD turbulence
We develop an analytic model of intermittent, three-dimensional, strong, reduced magnetohydrodynamic (RMHD) turbulence with zero cross helicity. We take the fluctuation amplitudes to have a log-Poisson distribution and incorporate into the model a new phenomenology of scale-dependent dynamic alignment between the Elsässer variables z{sup ±}. We find that the structure function 〈|Δz{sub λ}{sup ±}|{sup n}〉 scales as λ{sup 1−β{sup n}}, where Δz{sub λ}{sup ±} is the variation in z{sup ±} across a distance λ perpendicular to the magnetic field. We calculate the value of β to be ≃ 0.69 based on our assumption that the most intense coherent structures are two-dimensional with a volume filling factor ∝ λ. Two consequences of this structure-function scaling are that the total-energy power spectrum is ∝ k{sub ⊥}{sup −1.52} and the kurtosis of the fluctuations is ∝ λ{sup −0.27}. Our model resolves the problem that alignment angles defined in different ways exhibit different scalings. Specifically, we find that the energy-weighted average angle between the velocity and magnetic-field fluctuations is ∝ λ{sup 0.21}, the energy-weighted average angle between Δz{sup +} and Δz{sup −} is ∝ λ{sup 0.10}, and the average angle between Δz{sup +} and Δz{sup −} without energy weighting is ∝ [ln(L/λ)]{sup −1/2} when L/λ≫1, where L is the outer scale. We also carry out a direct numerical simulation of RMHD turbulence. The scalings in our model are similar to the scalings in this simulation as well as the structure-function scalings observed in the slow solar wind.