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

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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 . ISSN 0031-9007

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Official URL: http://dx.doi.org/10.1103/PhysRevLett.98.211101

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

Identification Number:

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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