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- W3105337024 abstract "The relationship between a decaying strong turbulence and the mirror instability in a slowly expanding plasma is investigated using two-dimensional hybrid expanding box simulations. We impose an initial ambient magnetic field perpendicular to the simulation box, and we start with a spectrum of large-scale, linearly-polarized, random-phase Alfvenic fluctuations which have energy equipartition between kinetic and magnetic fluctuations and vanishing correlation between the two fields. A turbulent cascade rapidly develops, magnetic field fluctuations exhibit a Kolmogorov-like power-law spectrum at large scales and a steeper spectrum at sub-ion scales. The imposed expansion (taking a strictly transverse ambient magnetic field) leads to generation of an important perpendicular proton temperature anisotropy that eventually drives the mirror instability. This instability generates large-amplitude, nonpropagating, compressible, pressure-balanced magnetic structures in a form of magnetic enhancements/humps that reduce the perpendicular temperature anisotropy." @default.
- W3105337024 created "2020-11-23" @default.
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- W3105337024 date "2017-04-05" @default.
- W3105337024 modified "2023-10-12" @default.
- W3105337024 title "Mirror Instability in the Turbulent Solar Wind" @default.
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- W3105337024 doi "https://doi.org/10.3847/1538-4357/aa67e0" @default.
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