Cascade models of anisotropic turbulence in magnetized plasma of solar wind
The model treats solar wind turbulence using discrete domains with rotational symmetry to describe anisotropic plasma flow. It introduces two characteristic time scales for energy transfer, leading to a bimodal cascade solution: a robust k-3/2 spectrum and a marginal k-5/3 spectrum. The system selects the faster cascade when energy flux is supercritical, causing localized phase transitions that explain observed decoupling between velocity and magnetic field spectra.