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Observational Evidence of How Magnetofluid Turbulence in the Solar Wind DissipatesThe solar wind appears to be a fully developed turbulent magnetofluid. As this magnetofluid expands into the heliosphere, it cools significantly less rapidly than would be expected of an adiabatically expanding gas. The evolution of the temperature with distance is roughly what would be expected if the turbulence dissipated by heating the thermal plasma. Several physical mechanisms have been proposed, including resonance absorption of waves and Landau damping. Recently, high-time resolution magnetic field data from the four Cluster spacecraft have illustrated damping of the fluctuations out to the electron inertial scale. Use of the wave telescope/k-filtering technique during two intervals of busrt mode data suggests that dissipation of the fluctuations is due to Landau damping, first on protons, then on electrons.
Document ID
20110015195
Acquisition Source
Goddard Space Flight Center
Document Type
Conference Paper
Authors
Goldstein, Melvyn L. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
August 25, 2013
Publication Date
August 15, 2011
Subject Category
Geophysics
Report/Patent Number
GSFC.ABS.4943.2011
Meeting Information
Meeting: International Space Plasma Symposium (ISPS) National Cheng Kung University
Location: Tainan
Country: Taiwan, Province of China
Start Date: August 15, 2011
End Date: August 19, 2011
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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