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Solar wind magnetic turbulence: Inferences from spectral shape

Treumann, R. A., W. Baumjohann, and Y. Narita (2016), Solar wind magnetic turbulence: Inferences from spectral shape, ArXiv, arXiv:1602.08605, 1-9.

Abstract
Differences between theoretical, numerical and observational determinations of spectral slopes of solar wind turbulence are interpreted in thermodynamical sense. Confirmations of turbulent Kolmogorov slopes in solar wind magnetic turbulence and magnetohydrodynamic simulations exhibit tiny differences. These are used to infer about the generation entropy in the turbulent cascade and estimating the anomalous turbulent collision frequency in the dissipative range as well as the average energy input in solar wind turbulence. Anomalous turbulent collision frequencies are obtained of the order of $\nu_{an}\approx 200$ Hz. The corresponding stationary energy input into solar wind magnetic turbulences into the Kolmogorov inertial range is obtained to be of the order of $\approx 47$ eV/s.
Further information
BibTeX
@article{id2130,
  author = {R. A. Treumann and W. Baumjohann and Y. Narita},
  journal = {ArXiv},
  month = {mar},
  pages = {1-9},
  title = {{Solar wind magnetic turbulence: Inferences from spectral shape}},
  volume = {arXiv:1602.08605},
  year = {2016},
  url = {http://adsabs.harvard.edu/abs/2016arXiv160208605T},
}
EndNote
%0 Journal Article
%A Treumann, R. A.
%A Baumjohann, W.
%A Narita, Y.
%D 2016
%V arXiv:1602.08605
%J ArXiv
%P 1-9
%T Solar wind magnetic turbulence: Inferences from spectral shape
%U http://adsabs.harvard.edu/abs/2016arXiv160208605T
%8 mar
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Printed 20. Aug 2019 17:57