On the 1/f spectrum in the solar wind and its connection with magnetic compressibility

Abstract

We discuss properties of Alfvénic fluctuations with large amplitude in plasmas characterised by low magnetic field compression. We note that in such systems power laws can not develop with arbitrarily steep slopes at large scales, i.e. when $|\delta \mathbf{B}|$ becomes of the order of the background field $|\mathbf{B}|$. In such systems there is a scale $l_0$ at which the spectrum has to break due to the condition of weak compressibility. A very good example of this dynamics is offered by solar wind fluctuations in Alfvénic fast streams, characterised by the property of constant field magnitude. We show here that the distribution of $\delta B=|\delta \mathbf{B}|$ in the fast wind displays a strong cut-off at $\delta B/|\mathbf{B}|\lesssim 2$, as expected for fluctuations bounded on a sphere of radius $B=|\mathbf{B}|$. This is also associated with a saturation of the rms of the fluctuations at large scales and introduces a specific length $l_0$ above which the amplitude of the fluctuations becomes independent on the scale $l$. Consistent with that, the power spectrum at $l>l_0$ is characterised by a -1 spectral slope, as expected for fluctuations that are scale-independent. Moreover, we show that the spectral break between the 1/f and inertial range in solar wind spectra indeed corresponds to the scale $l_0$ at which $⟨\delta B/B⟩\sim 1$. Such a simple model provides a possible alternative explanation of magnetic spectra observed in interplanetary space, also pointing out the inconsistency for a plasma to simultaneously maintain $|\mathbf{B}|\sim$const. at arbitrarily large scales and satisfy a Kolmogorov scaling.

6 pages, 5 figures, Accepted by The Astrophysical Journal Letters

References in corpus (2)

• Ion kinetic energy conservation and magnetic field strength constancy in multi-fluid solar wind Alfvénic turbulence
• Nature of the MHD and kinetic scale turbulence in the magnetosheath of Saturn: Cassini observations

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