Turbulence, Spatial Transport, and Heating of the Solar Wind | Zendy

W. H. Matthaeus | Zendy; G. P. Zank | Zendy; C. W. Smith | Zendy; S. Oughton | Zendy

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Turbulence, Spatial Transport, and Heating of the Solar Wind

Author(s) -

W. H. Matthaeus,

G. P. Zank,

C. W. Smith,

S. Oughton

Publication year - 1999

Publication title -

physical review letters

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 3.688

H-Index - 673

eISSN - 1079-7114

pISSN - 0031-9007

DOI - 10.1103/physrevlett.82.3444

Subject(s) - physics , solar wind , turbulence , plasma , magnetohydrodynamic turbulence , spacecraft , computational physics , magnetic field , magnetohydrodynamics , mechanics , astrophysics , astronomy , nuclear physics , quantum mechanics

A phenomenological theory describes radial evolution of plasma turbulence in the solar wind from 1 to 50 astronomical units. The theory includes a simple closure for local anisotropic magnetohydrodynamic turbulence, spatial transport, and driving by large-scale shear and pickup ions. Results compare well to plasma and magnetic field data from the Voyager 2 spacecraft, providing a basis for a concise, tractable description of turbulent energy transport in a variety of astrophysical plasmas

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