Self-Similar Signature of the Active Solar Corona within the Inertial Range of Solar-Wind Turbulence

K. Kiyani, S. C. Chapman, B. Hnat, and R. M. Nicol
Phys. Rev. Lett. 98, 211101 – Published 23 May 2007

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.

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  • Received 14 February 2007

DOI:https://doi.org/10.1103/PhysRevLett.98.211101

©2007 American Physical Society

Authors & Affiliations

K. Kiyani*, S. C. Chapman, B. Hnat, and R. M. Nicol

  • Centre for Fusion, Space and Astrophysics; Department of Physics, University of Warwick, Coventry CV4 7AL, United Kingdom

  • *Electronic address: k.kiyani@warwick.ac.uk

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Vol. 98, Iss. 21 — 25 May 2007

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