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dc.contributor.authorMatthaeus, William H.
dc.contributor.authorZank, Gary P.
dc.contributor.authorSmith, Charles W.
dc.contributor.authorOughton, Sean
dc.date.accessioned2014-04-03T20:21:07Z
dc.date.available2014-04-03T20:21:07Z
dc.date.copyright1999-04
dc.date.issued1999
dc.identifier.citationMatthaeus, W., Zank, G., Smith, C., & Oughton, S. (1999). Turbulence, Spatial Transport, and Heating of the Solar Wind. Physical Review Letters, 82(17), 3444-3447.en_NZ
dc.identifier.urihttps://hdl.handle.net/10289/8611
dc.description.abstractA 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.en_NZ
dc.format.mimetypeapplication/pdf
dc.language.isoenen_NZ
dc.publisherThe American Physical Societyen_NZ
dc.relation.ispartofPhys. Rev. Lett.
dc.rights© 1999 The American Physical Societyen_NZ
dc.subjectturbulenceen_NZ
dc.subjectsolar winden_NZ
dc.titleTurbulence, spatial transport, and heating of the solar winden_NZ
dc.typeJournal Articleen_NZ
dc.identifier.doi10.1103/physrevlett.82.3444en_NZ
dc.relation.isPartOfPhysical Review Lettersen_NZ
pubs.begin-page3444en_NZ
pubs.elements-id28187
pubs.end-page3447en_NZ
pubs.issue17en_NZ
pubs.volume82en_NZ


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