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Estimation of the energy cascade rate in the inertial range of solar windturbulence has been done so far mostly within the incompressiblemagnetohydrodynamics (MHD) theory. Here, we go beyond that approximation toinclude plasma compressibility using a reduced form of a recently derived exactlaw for compressible, isothermal MHD turbulence. Using in-situ data from theTHEMIS/ARTEMIS spacecraft in the fast and slow solar wind, we investigate indetail the role of the compressible fluctuations in modifying the energycascade rate with respect to the prediction of the incompressible MHD model. Inparticular, we found that the energy cascade rate: i) is amplified particularlyin 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 levelof spatial anisotropy. Other features of solar wind turbulence are discussedalong with their comparison with previous studies that used incompressible orheuristic (non exact) compressible MHD models.

Energy Cascade Rate In Compressible Fast And Slow Solar Wind Turbulence