Heating and cooling of protons by turbulence-driven ion cyclotron waves in the fast solar wind

Physics – Plasma Physics

Scientific paper

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Space Plasma Physics: Turbulence, Space Plasma Physics: Numerical Simulation Studies, Interplanetary Physics: Mhd Waves And Turbulence

Scientific paper

The effects of parallel propagating nondispersive ion cyclotron waves on the solar wind plasma are investigated in an attempt to reproduce the observed proton temperature anisotropy, namely, Tp⊥>>Tp∥ in the inner corona and Tp⊥>Tp∥. The waves provide the mechanism for the extraction of energy from the parallel direction to feed into the perpendicular direction. In our models, both Kolmogorov and Kraichnan dissipation rates yield Tp⊥>>Tp∥ in the corona, in agreement with inferences from recent ultraviolet coronal measurements, and predict temperatures at 1 AU which match in situ observations. The models also reproduce the inferred rapid acceleration of the fast solar wind in the inner corona and flow speeds and particle fluxes measured at 1 AU. Since this mechanism does not provide direct energy to the electrons, and the electron-proton coupling is not sufficient to heat the electrons to temperatures at or above 106K, this model yields electron temperatures which are much cooler than those currently inferred from observations.

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