Self-similar signature of the active solar corona within the inertial range of solar wind turbulence

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dc.creatorKiyani, K.
dc.creatorChapman, S. C.
dc.creatorHnat, B.
dc.creatorNicol, R. M.
dc.date2007-02-14
dc.date2007-05-25
dc.date.accessioned2026-07-07T08:03:10Z
dc.date.available2026-07-07T08:03:10Z
dc.descriptionWe quantify the scaling of magnetic energy density in the inertial range of solar wind turbulence seen in-situ at 1AU with respect to solar activity. At solar maximum, when the coronal magnetic field is dynamic and topologically complex, we find self-similar scaling in the solar wind, whereas at solar mimimum, when the coronal fields are more ordered, we find multifractality. This quantifies the solar wind signature that is of direct coronal origin, and distinguishes it from that of local MHD turbulence, with quantitative implications for our understanding of coronal heating of the solar wind.
dc.description5 pages, 7 figures, accepted in Phys. Rev. Lett
dc.identifierhttps://arxiv.org/abs/physics/0702123
dc.identifierhttp://arxiv.org/abs/physics/0702123
dc.identifierPhys. Rev. Lett. 98, 211101 (2007)
dc.identifierdoi:10.1103/PhysRevLett.98.211101
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/129483
dc.subjectSpace Physics
dc.subjectFluid Dynamics
dc.titleSelf-similar signature of the active solar corona within the inertial range of solar wind turbulence
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