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Solar Wind Heating by the Turbulent Energy Cascade

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Turbulence in the Solar Wind

Part of the book series: Lecture Notes in Physics ((LNP,volume 928))

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Abstract

The Parker theory (Parker 1958; Parker 1963) predicts an adiabatic expansion of the solar wind from the hot corona without further heating. For such a model, the proton temperature T(r) should decrease with the heliocentric distance r as T(r) ∼ r −4∕3.

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Notes

  1. 1.

    For a discussion on non-turbulent mechanism of solar wind heating cf. Tu and Marsch (1995a).

  2. 2.

    Of course, this is based on classical turbulence. As said before, in the solar wind the dissipative term is unknown, even if it might happens at very small kinetic scales.

  3. 3.

    It is worthwhile to remark that a turbulent fluid flows is out of equilibrium, say the cascade requires the injection of energy (input) and a dissipation mechanism (output), usually lying on well separated scales, along with a transfer of energy. Without input and output, the nonlinear term of equations works like an energy redistribution mechanism towards an equilibrium in the wave vectors space. This generates an equilibrium energy spectrum which should in general be the same as that obtained when the cascade is at work (cf., e.g., Frisch et al. 1975). However, even if the turbulent spectra could be anticipated by looking at the equilibrium spectra, the physical mechanisms are different. Of course, this should also be the case for the Hall MHD.

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Authors and Affiliations

  1. Fisica dei Plasmi Spaziali, INAF - Istituto di Astrofisica e Planetologia Spaziali, Roma, Italy

    Roberto Bruno

  2. Dipartimento di Fisica, Università della Calabria, Rende (CS), Italy

    Vincenzo Carbone

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  2. Vincenzo Carbone
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Bruno, R., Carbone, V. (2016). Solar Wind Heating by the Turbulent Energy Cascade. In: Turbulence in the Solar Wind. Lecture Notes in Physics, vol 928. Springer, Cham. https://doi.org/10.1007/978-3-319-43440-7_8

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