Turbulent cascade and energy transfer rate in a solar coronal mass ejection

Abstract

Turbulence properties are examined before, during and after a coronal mass ejection (CME) detected by the6Wind spacecraft on July 2012. The power-law scaling of the structure functions, providing information on the7power spectral density and flatness of the velocity, magnetic filed and density fluctuations, were examined. The8third-order moment scaling law for incompressible, isotropic magnetohydrodynamic turbulence was observed9in the preceding and trailing solar wind, as well as in the CME sheath and magnetic cloud. This suggests that10the turbulence could develop sufficiently after the shock, or that turbulence in the sheath and cloud regions11was robustly preserved even during the mixing with the solar wind plasma. The turbulent energy transfer rate12was thus evaluated in each of the regions. The CME sheath shows an increase of energy transfer rate, as13expected from the lower level of Alfvénic fluctuations and suggesting the role of the shock-wind interaction as14an additional source of energy for the turbulent cascade.

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Cited by in corpus (7)

• Helios 2 observations of solar wind turbulence decay in the inner heliosphere
• Turbulence Properties of Interplanetary Coronal Mass Ejections in the Inner Heliosphere: Dependence on Proton Beta and Flux Rope Structure
• Cross helicity of interplanetary coronal mass ejections at 1 au
• Turbulence, intermittency and cross-scale energy transfer in an interplanetary coronal mass ejection
• Intermittency in Interplanetary Coronal Mass Ejections Observed by Parker Solar Probe and Solar Orbiter
• The effects of expansion and turbulence on the interplanetary evolution of a magnetic cloud
• Numerical investigation of particle acceleration at interplanetary shocks: diffusive and superdiffusive scenarios