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dc.contributor.authorMatthaeus, William H.
dc.contributor.authorOughton, Sean
dc.contributor.authorOsman, Kareem T.
dc.contributor.authorServidio, Sergio
dc.contributor.authorWan, Minping
dc.contributor.authorGary, S.P.
dc.contributor.authorShay, M.A.
dc.contributor.authorValentini, F.
dc.contributor.authorRoytershteyn, V.
dc.contributor.authorKarimabadi, H.
dc.contributor.authorChapman, S.C.
dc.date.accessioned2014-12-04T20:36:29Z
dc.date.available2014-08-01
dc.date.available2014-12-04T20:36:29Z
dc.date.issued2014-08-01
dc.identifierhttp://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=000339115800072&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=361a7c8f0a33fd6c66ab5b004b3aea5f
dc.identifierARTN 155
dc.identifier.citationMatthaeus, W. H., Oughton, S., Osman, K. T., Servidio, S., Wan, M., Gary, S. P., … Chapman, S. C. (2014). Nonlinear and linear timescales near kinetic scales in solar wind turbulence. Astrophysical Journal, 790(2):155. http://doi.org/10.1088/0004-637X/790/2/155en
dc.identifier.issn1538-4357
dc.identifier.urihttps://hdl.handle.net/10289/8898
dc.description.abstractThe application of linear kinetic treatments to plasma waves, damping, and instability requires favorable inequalities between the associated linear timescales and timescales for nonlinear (e.g., turbulence) evolution. In the solar wind these two types of timescales may be directly compared using standard Kolmogorov-style analysis and observational data. The estimated local (in scale) nonlinear magnetohydrodynamic cascade times, evaluated as relevant kinetic scales are approached, remain slower than the cyclotron period, but comparable to or faster than the typical timescales of instabilities, anisotropic waves, and wave damping. The variation with length scale of the turbulence timescales is supported by observations and simulations. On this basis the use of linear theory—which assumes constant parameters to calculate the associated kinetic rates—may be questioned. It is suggested that the product of proton gyrofrequency and nonlinear time at the ion gyroscales provides a simple measure of turbulence influence on proton kinetic behavior.
dc.format.extent? - ? (8)
dc.format.mimetypeapplication/pdf
dc.languageen
dc.publisherAmerican Astronomical Society
dc.rightsThis article is published in the Astrophysical Journal. © 2014 The American Astronomical Society
dc.subjectScience & Technology
dc.subjectPhysical Sciences
dc.subjectAstronomy & Astrophysics
dc.subjectASTRONOMY & ASTROPHYSICS
dc.subjectmagnetohydrodynamics (MHD)
dc.subjectsolar wind
dc.subjectSun: corona
dc.subjectturbulence
dc.subjectMEAN MAGNETIC-FIELD
dc.subject3-DIMENSIONAL MAGNETOHYDRODYNAMIC TURBULENCE
dc.subjectTEST PARTICLE-ACCELERATION
dc.subjectIN-CELL SIMULATIONS
dc.subjectHYDROMAGNETIC WAVES
dc.subjectALFVEN WAVES
dc.subjectENERGY CASCADE
dc.subjectPLASMA
dc.subjectMHD
dc.subjectFLUCTUATIONS
dc.titleNonlinear and linear timescales near kinetic scales in solar wind turbulence
dc.typeJournal Article
dc.identifier.doi10.1088/0004-637X/790/2/155
dc.relation.isPartOfAstrophysical Journal
pubs.begin-page155en_NZ
pubs.elements-id84995
pubs.end-page155en_NZ
pubs.issue2
pubs.publication-statusPublished
pubs.volume790
uow.identifier.article-noARTN 155en_NZ


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