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Solar wind turbulence: Advances in observations and theory

Published online by Cambridge University Press:  08 June 2011

J. J. Podesta
J. J. Podesta*
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM, 87545, USA email: jpodesta@solar.stanford.edu
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Abstract

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Observations of plasma and magnetic field fluctuations in the solar wind provide a valuable source of information for the study of turbulence in collisionless astrophysical plasmas. Scientific data collected by various spacecraft over the last few decades has fueled steady progress in this field. Theoretical models, numerical simulations, and comparisons between theory and experiment have also contributed greatly to these advances. This review highlights some recent advances on the observational side including measurements of the anisotropy of inertial range fluctuations as revealed by the different scaling laws parallel and perpendicular to the mean magnetic field, measurements of the normalized cross-helicity spanning the entire inertial range which demonstrate that this quantity is scale invariant, and improved measurements of the spectrum of magnetic field fluctuations in the dissipation range that show a spectral break near the lengthscale of the electron gyro-radius. The theoretical implications of these results and comparisons between theory and observations are briefly summarized.

Keywords

Solar windturbulenceinterplanetary mediumwaves
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 295 - 301
Copyright
Copyright © International Astronomical Union 2011

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