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Kinetic scale turbulence and dissipation in the solar wind: key observational results and future outlook.

ABSTRACT: Turbulence is ubiquitous in the solar wind. Turbulence causes kinetic and magnetic energy to cascade to small scales where they are eventually dissipated, adding heat to the plasma. The details of how this occurs are not well understood. This article reviews the evidence for turbulent dissipation and examines various diagnostics for identifying solar wind regions where dissipation is occurring. We also discuss how future missions will further enhance our understanding of the importance of turbulence to solar wind dynamics.

SUBMITTER: Goldstein ML

PROVIDER: S-EPMC4394679 | biostudies-other | 2015 May

REPOSITORIES: biostudies-other

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Kinetic scale turbulence and dissipation in the solar wind: key observational results and future outlook.

Goldstein M L ML Wicks R T RT Perri S S Sahraoui F F

Philosophical transactions. Series A, Mathematical, physical, and engineering sciences 20150501 2041

Turbulence is ubiquitous in the solar wind. Turbulence causes kinetic and magnetic energy to cascade to small scales where they are eventually dissipated, adding heat to the plasma. The details of how this occurs are not well understood. This article reviews the evidence for turbulent dissipation and examines various diagnostics for identifying solar wind regions where dissipation is occurring. We also discuss how future missions will further enhance our understanding of the importance of turbul ...[more]

PMID: 25848084

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