Lognormal and multifractal distributions of the heliospheric magnetic field
Article first published online: 20 SEP 2012
This paper is not subject to U.S. copyright. Published in 2001 by the American Geophysical Union.
Journal of Geophysical Research: Space Physics (1978–2012)
Volume 106, Issue A8, pages 15917–15927, 1 August 2001
How to Cite
2001), Lognormal and multifractal distributions of the heliospheric magnetic field, J. Geophys. Res., 106(A8), 15917–15927, doi:10.1029/2000JA000107.(
- Issue published online: 20 SEP 2012
- Article first published online: 20 SEP 2012
- Manuscript Accepted: 24 JUL 2000
- Manuscript Received: 1 MAY 2000
The heliospheric magnetic field strength B fluctuates appreciably over a large range of scales in the region from 1 AU to at least 30 AU and throughout the solar cycle. The fluctuations are often extreme and intermittent. For example, the distributions of hour averages of these parameters are usually lognormal to a good approximation, the long tail representing extreme events. The fluctuations can often be described by a multifractal distribution on scales from approximately 12 hours to 27 days or more, reflecting scaling symmetries of various moments of the fluctuations. Statistical variations, burstiness, extreme values, and clusters on various scales are ubiquitous in the time series describing the magnetic field. These properties can be described quantitatively, although not uniquely. Models of the solar wind should at least be consistent with these results. Ultimately, there is a need for physical models that can explain the statistical properties of the observed large-scale fluctuations.