Physics
Scientific paper
Aug 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....8.3322s&link_type=abstract
Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int
Physics
1
Scientific paper
Magnetic fluctuation power spectra in the solar wind are commonly observed to have a power-law form with a spectral index s = 5/3 at frequencies lower than about 1 Hz. This characteristic feature of magnetic fluctuation spectra defines what is called the inertial range and may be described, in wavenumber space, by Kolmogorov diffusion. For higher frequencies, it has been suggested that collisionless damping of Alfv´en and magnetosonic waves leads to steeper power-laws; this regime is sometimes labeled as the dissipation range. Here we argue, based on numerical calculations, that it is more likely that the observed steeper powerlaws result from an increase in the wavenumber diffusion rate caused by whistler-like dispersion than from collisionless damping. The calculations lead to the prediction, that this broken power-law feature of magnetic fluctuation spectra is only observable in low-βp plasmas.
Gary Peter S.
Li Handong
Stawicki Olaf
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