Scaling anisotropy of the power in parallel and perpendicular components of the solar wind magnetic field

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dc.contributor.authorForman, Miriam A.
dc.contributor.authorWicks, Robert T.
dc.contributor.authorHorbury, Timothy S.
dc.contributor.authorOughton, Sean
dc.coverage.spatialBig Island, Hawaiien_NZ
dc.date.accessioned2013-09-18T04:09:40Z
dc.date.available2013-09-18T04:09:40Z
dc.date.issued2013
dc.description.abstractPower spectra of the components of the magnetic field parallel (Pzz) and perpendicular (Pzz+Pyy) to the local mean magnetic field direction were determined by wavelet methods from Ulysses’ MAG instrument data during eighteen 10-day segments of its first North Polar pass at high latitude at solar minimum in 1995. The power depends on frequency f and the angle θ between the solar wind direction and the local mean field, and with distance from the Sun. This data includes the solar wind whose total power (Pxx + Pyy + Pzz) in magnetic fluctuations we previously reported depends on f and the angle θ nearly as predicted by the GS95 critical balance model of strong incompressible MHD turbulence. Results at much wider range of frequencies during six evenly-spaced 10-day periods are presented here to illustrate the variability and evolution with distance from the Sun. Here we investigate the aniso tropic scaling of Pzz(f,θ) in particular because it is a reduced form of the Poloidal (pseudo-Alfvenic) component of the (incompressible) fluctuations. We also report the much larger Pxx(f,θ)+Pyy(f,θ) which is (mostly) reduced from the Toroidal (Alfvenic, i.e., perpendicular to both B and k) fluctuations, and comprises most of the total power. These different components of the total power evolve and scale differently in the inertial range. We compare these elements of the magnetic power spectral tensor with “critical balance” model predictions.en_NZ
dc.format.mimetypeapplication/pdf
dc.identifier.citationForman, M. A., Wicks, R. T., Horbury, T. S., & Oughton, S. (2013). Scaling anisotropy of the power in parallel and perpendicular components of the solar wind magnetic field. AIP Conference Proceedings, 1539, 167-170.en_NZ
dc.identifier.doi10.1063/1.4811014en_NZ
dc.identifier.urihttps://hdl.handle.net/10289/8002
dc.language.isoenen_NZ
dc.publisherAmerican Institute of Physicsen_NZ
dc.relation.isPartOfProc 13th International Solar Wind Conference 2012en_NZ
dc.relation.replaceshttps://hdl.handle.net/10289/8002
dc.relation.replaces10289/8002
dc.relation.urihttp://proceedings.aip.org/resource/2/apcpcs/1539/1/167_1?isAuthorized=noen_NZ
dc.rightsCopyright © 2012 American Institute of Physics.en_NZ
dc.sourceSolar Wind 13en_NZ
dc.subjectastrophysical plasmaen_NZ
dc.subjectinterplanetary magnetic fieldsen_NZ
dc.subjectplasma Alfven wavesen_NZ
dc.subjectplasma magnetohydrodynamicsen_NZ
dc.subjectsolar winden_NZ
dc.titleScaling anisotropy of the power in parallel and perpendicular components of the solar wind magnetic fielden_NZ
dc.typeConference Contributionen_NZ
pubs.begin-page167en_NZ
pubs.elements-id83914
pubs.end-page170en_NZ
pubs.finish-date2012-06-22en_NZ
pubs.start-date2012-06-17en_NZ
pubs.volume1539en_NZ
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