Where Does Fluid-like Turbulence Break Down in the Solar Wind?

Details Where Does Fluid-like Turbulence Break Down in the Solar Wind? Where Does Fluid-like Turbulence Break Down in the Solar Wind?

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...725l..52p&link_type=abstract

The Astrophysical Journal Letters, Volume 725, Issue 1, pp. L52-L55 (2010).

Astronomy and Astrophysics

Astronomy

3

Interplanetary Medium, Turbulence

Scientific paper

Power spectra of the magnetic field in solar wind display a Kolmogorov law f -5/3 at intermediate range of frequencies f, say within the inertial range. Two spectral breaks are also observed: one separating the inertial range from an f -1 spectrum at lower frequencies, and another one between the inertial range and an f -7/3 spectrum at higher frequencies. The breaking of fluid-like turbulence at high frequencies has been attributed to either the occurrence of kinetic Alfvén wave fluctuations above the ion-cyclotron frequency or to whistler turbulence above the frequency corresponding to the proton gyroradius. Using solar wind data, we show that the observed high-frequency spectral break seems to be independent of the distance from the Sun, and then of both the ion-cyclotron frequency and the proton gyroradius. We suppose that the observed high-frequency break could be either caused by a combination of different physical processes or associated with a remnant signature of coronal turbulence.

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