huang-mhd-turbulence

The expanding-box model is a simulation framework for MHD turbulence that accounts for the spherical expansion of the solar wind. It helps analyze anisotropic scaling and residual energy evolution as plasma propagates outward.

You can compare MHD turbulence simulations with Parker Solar Probe observations by generating synthetic observables from expanding-box model outputs and matching them against spacecraft data for intermittency and anisotropic scaling.

Yes, you need prior knowledge of MHD turbulence theory and simulation techniques. The workflow focuses on research-level analysis of residual energy, intermittency, and anisotropic scaling rather than introductory concepts.

Residual energy in solar wind MHD turbulence is the difference between kinetic and magnetic energy fluctuations. Analyzing it with the expanding-box model reveals how energy partition evolves during solar wind expansion.

Intermittency causes localized turbulent bursts that disrupt self-similar scaling, making anisotropic scaling in solar wind MHD turbulence dependent on scale and direction. The expanding-box model captures these effects for comparison with Solar Orbiter data.