Validity of using Elsässer variables to study the interaction of compressible solar wind fluctuations with a coronal mass ejection

Abstract

Alfvénic fluctuations, as modelled by the non-linear interactions of Alfvén waves of various scales, are seen to dominate solar wind turbulence. However, there is also a non-negligible component of non-Alfvénic fluctuations. The Elsässer formalism, which is central to the study of Alfvénic turbulence due to its ability to differentiate between parallel and anti-parallel Alfvén waves, cannot strictly separate wavemodes in the presence of compressive magnetoacoustic waves. In this study, we analyse the deviations generated in the Elsässer formalism as density fluctuations are naturally generated through the propagation of a linearly polarised Alfvén wave. The study was performed in the context of a coronal mass ejection (CME) propagating through the solar wind, which enables the creation of two solar wind regimes, pristine wind and a shocked CME sheath, where the Elsässer formalism can be evaluated. In these two regimes we studied the deviations of the Elsässer formalism in separating parallel and anti-parallel components of Alfvénic solar wind perturbations generated by small-amplitude density fluctuations. We used an ideal 2.5D magnetohydrodynamic (MHD) model with an adiabatic equation of state. An Alfvén pump wave was injected into the quiet solar wind by perturbing the transverse magnetic field and velocity components. This wave subsequently generates density fluctuations through the ponderomotive force. A CME was injected by inserting a flux-rope modelled as a magnetic island into the quasi-steady solar wind. The presence of density perturbations creates an approximately 10% deviation in the Elsässer variables and reflection coefficient for the Alfvén waves as well as a deviation of approximately 0.1 in the cross helicity in regions containing both parallel and anti-parallel fluctuations.

arXiv commentAccepted for publication in Astronomy and Astrophysics

References in corpus (20)

• Astrophysical gyrokinetics: kinetic and fluid turbulent cascades in magnetized weakly collisional plasmas
• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence
• Alfven Wave Solar Model (AWSoM): Coronal Heating
• On the Generation, Propagation, and Reflection of Alfven Waves from the Solar Photosphere to the Distant Heliosphere
• Alfven Waves and Turbulence in the Solar Atmosphere and Solar Wind
• Recent progress in astrophysical plasma turbulence from solar wind observations
• Incorporating Kinetic Physics into a Two-Fluid Solar-Wind Model with Temperature Anisotropy and Low-Frequency Alfven-Wave Turbulence
• Weak compressible magnetohydrodynamic turbulence in the solar corona
• Heating and Acceleration of the Fast Solar Wind by Alfvén Wave Turbulence
• Reflection-driven MHD turbulence in the solar atmosphere and solar wind
• Frequency-dependent Alfvén-wave propagation in the solar wind: Onset and suppression of parametric decay instability
• Coronal Heating and Acceleration of the High/Low-Speed Solar Wind by Fast/Slow MHD Shock Trains
• Evolving waves and turbulence in the outer corona and inner heliosphere: the accelerating expanding box
• Stochastic proton heating by kinetic-Alfvén-wave turbulence in moderately high-$\beta$ plasmas
• On the Existence of Fast Modes in Compressible Magnetohydrodynamic Turbulence
• The nature of Elsässer variables in compressible MHD
• Cross helicity of interplanetary coronal mass ejections at 1 au
• Nature and Scalings of Density Fluctuations of Compressible MHD Turbulence with Applications to the Solar Wind
• Flux-tube-dependent propagation of Alfvén waves in the solar corona
• Modelling the interaction of Alfvénic fluctuations with coronal mass ejections in the low solar corona