Influence of the heliospheric current sheet on the evolution of solar wind turbulence

Abstract

The effects of the heliospheric current sheet (HCS) on the evolution of Alfvénic turbulence in the solar wind are studied using MHD simulations incorporating the expanding-box-model (EBM). The simulations show that near the HCS, the Alfvénicity of the turbulence decreases as manifested by lower normalized cross helicity and larger excess of magnetic energy. The numerical results are supported by a superposed-epoch analysis using OMNI data, which shows that the normalized cross helicity decreases inside the plasma sheet surrounding HCS, and the excess of magnetic energy is significantly enhanced at the center of HCS. Our simulation results indicate that the decrease of Alfvénicity around the HCS is due to the weakening of radial magnetic field and the effects of the transverse gradient in the background magnetic field. The magnetic energy excess in the turbulence may be a result of the loss of Alfvénic correlation between velocity and magnetic field and the faster decay of transverse kinetic energy with respect to magnetic energy in a spherically expanding solar wind.

References in corpus (8)

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Cited by in corpus (6)

• Magnetic field intermittency in the solar wind: PSP and SolO observations ranging from the Alfven region out to 1 AU
• Preferential Proton over Electron heating from coherent structures during the first perihelion of Parker Solar Probe
• Analytic Model and Magnetohydrodynamic Simulations of Three-dimensional Magnetic Switchbacks
• Imbalanced Turbulence Modified by Large-scale Velocity Shears in the Solar Wind
• Evolution of MHD turbulence in the expanding solar wind: residual energy and intermittency
• Does Turbulence along the Coronal Current Sheet Drive Ion Cyclotron Waves?