On the fractal nature of the magnetic field energy density in the solar wind

Hnat, B.; Chapman, S.C.; Kiyani, K.; Rowlands, G.; Watkins, Nicholas W.. 2007 On the fractal nature of the magnetic field energy density in the solar wind. Geophysical Research Letters, 34 (15), L15108. 4, pp. https://doi.org/10.1029/2007GL029531

Before downloading, please read NORA policies.

Text 2007GL029531.pdf - Published Version Restricted to NERC registered users only Download (189kB) | Request a copy

Abstract/Summary

The solar wind exhibits scaling typical of intermittent turbulence in the statistics of in situ fluctuations in both the magnetic and velocity fields. Intriguingly, quantities not directly accessed by theories of ideal, incompressible, MHD turbulence, such as magnetic energy density, B-2, nevertheless show evidence of simple fractal (self-affine) statistical scaling. We apply a novel statistical technique which is a sensitive discriminator of fractality to the B-2 timeseries from WIND and ACE. We show that robust fractal behaviour occurs at solar maximum and determine the scaling exponents. The probability density function (PDF) of fluctuations at solar maximum and minimum are distinct. Power law tails are seen at maximum, and the PDF is reminiscent of a Levy flight.

Item Type:	Publication - Article
Digital Object Identifier (DOI):	https://doi.org/10.1029/2007GL029531
Programmes:	BAS Programmes > Global Science in the Antarctic Context (2005-2009) > Natural Complexity Programme
ISSN:	0094-8276
NORA Subject Terms:	Physics Atmospheric Sciences
Date made live:	08 Mar 2011 08:47 +0 (UTC)
URI:	https://nora.nerc.ac.uk/id/eprint/11754

Actions (login required)

View Item

Document Downloads

More statistics for this item...