Abstract
The whole heliosphere is permeated by the solar wind, a supersonic and super-Alfvénic plasma flow of solar origin which continuously expands into the heliosphere. This medium offers the best opportunity to study directly collisionless plasma phenomena, mainly at low frequencies where large-amplitude fluctuations have been observed. During its expansion, the solar wind develops a strong turbulent character, which evolves towards a state that resembles the well known hydrodynamic turbulence described by Kolmogorov (1941, 1991). Because of the presence of a strong magnetic field carried by the wind, low-frequency fluctuations in the solar wind are usually described within a magnetohydrodynamic (MHD, hereafter) benchmark (Kraichnan 1965; Biskamp 1993; Tu and Marsch 1995; Biskamp 2003; Petrosyan et al. 2010). However, due to some peculiar characteristics, the solar wind turbulence contains some features hardly classified within a general theoretical framework.
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This concept will be explained better in the next sections.
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Bruno, R., Carbone, V. (2016). Introduction. In: Turbulence in the Solar Wind. Lecture Notes in Physics, vol 928. Springer, Cham. https://doi.org/10.1007/978-3-319-43440-7_1
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