Radial evolution of cross helicity at low and high latitudes in the solar wind

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dc.contributor.authorBreech, Ben
dc.contributor.authorMatthaeus, William H.
dc.contributor.authorMinnie, J.
dc.contributor.authorOughton, Sean
dc.contributor.authorParhi, S.
dc.contributor.authorBieber, J.W.
dc.contributor.authorBavassano, B.
dc.date.accessioned2014-04-02T21:27:36Z
dc.date.available2014-04-02T21:27:36Z
dc.date.issued2005
dc.description.abstractWe employ a turbulence transport theory to the radial evolution of the solar wind at both low and high latitudes. The theory includes cross helicity, magnetohydrodynamic (MHD) turbulence, and driving by shear and pickup ions. The radial decrease of cross helicity, observed in both low and high latitudes, can be accounted for by including sufficient shear driving to overcome the tendency of MHD turbulence to produce Alfvénic states. The shear driving is weaker at high latitudes leading to a slower evolution. Model results are compared with observations from Ulysses and Voyager.en_NZ
dc.format.mimetypeapplication/pdf
dc.identifier.citationBreech, B., Matthaecus, W. H., Minnie, J., Oughton, S., Parhi, S.,…, Bavassano, B. (2005). In Proceedings of the Solar Wind 11 / SOHO 16, Connecting Sun and Heliosphere Conference (ESA SP-592).en_NZ
dc.identifier.urihttps://hdl.handle.net/10289/8595
dc.language.isoenen_NZ
dc.subjectMHD turbulenceen_NZ
dc.titleRadial evolution of cross helicity at low and high latitudes in the solar winden_NZ
dc.typeConference Contributionen_NZ
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