Kiyani, K., Chapman, Sandra C., Hnat, B. and Nicol, Ruth Mary (2007) Self-similar signature of the active solar corona within the inertial range of solar-wind turbulence. Physical Review Letters, Vol.98 . doi:10.1103/PhysRevLett.98.211101

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Abstract

We quantify the scaling of magnetic energy density in the inertial range of solar-wind turbulence seen
in situ at 1 AU 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
minimum, 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 coronal heating of the solar wind.

Item Type:	Journal Article
Subjects:	Q Science > QC Physics
Divisions:	Faculty of Science > Physics
Library of Congress Subject Headings (LCSH):	Geophysics -- Data processing, Solar wind, Sun -- Corona
Journal or Publication Title:	Physical Review Letters
Publisher:	American Physical Society
ISSN:	0031-9007
Official Date:	23 May 2007
Dates:	Date Event 23 May 2007 Published
Volume:	Vol.98
DOI:	10.1103/PhysRevLett.98.211101
Status:	Peer Reviewed
Access rights to Published version:	Restricted or Subscription Access
Funder:	Particle Physics and Astronomy Research Council (Great Britain) (PPARC)

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