Spatiotemporal dynamics of nonparallel transport of magnetohydrodynamic turbulence by the solar wind

Specifically for solar wind plasma, numerical methods are used to study the nonlinear dynamics of perpendicular magnetohydrodynamic (MHD) turbulence, which generates waves of all types propagating obliquely to the interplanetary magnetic field. It is shown that the leading edge of the fast magnetosonic pulse forms a shock wave, and that the trailing edge is stretched over a long distance during the formative stage. The dependence of the amplitude of the slow magnetosonic wave on the ratio of the sound and Alfven velocities is studied (V-s/V-A much less than 1). The effect of the fast solar-wind velocity on the nonlinear conversion of MHD waves is examined. A qualitative difference in the dynamics of strongly nonlinear Alfven pulses propagating strictly parallel and obliquely to the external magnetic field is observed.