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• W3100156583 abstract "Estimation of the energy cascade rate in the inertial range of solar wind turbulence has been done so far mostly within the incompressible magnetohydrodynamics (MHD) theory. Here, we go beyond that approximation to include plasma compressibility using a reduced form of a recently derived exact law for compressible, isothermal MHD turbulence. Using in-situ data from the THEMIS/ARTEMIS spacecraft in the fast and slow solar wind, we investigate in detail the role of the compressible fluctuations in modifying the energy cascade rate with respect to the prediction of the incompressible MHD model. In particular, we found that the energy cascade rate: i) is amplified particularly in the slow solar wind; ii) exhibits weaker fluctuations in spatial scales, which leads to a broader inertial range than the previous reported ones; iii) has a power law scaling with the turbulent Mach number; iv) has a lower level of spatial anisotropy. Other features of solar wind turbulence are discussed along with their comparison with previous studies that used incompressible or heuristic (non exact) compressible MHD models." @default.
• W3100156583 created "2020-11-23" @default.
• W3100156583 creator A5044640403 @default.
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• W3100156583 date "2017-03-17" @default.
• W3100156583 modified "2023-10-07" @default.
• W3100156583 title "Energy Cascade Rate in Compressible Fast and Slow Solar Wind Turbulence" @default.
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• W3100156583 doi "https://doi.org/10.3847/1538-4357/aa603f" @default.
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