Phase mixing and the 1/f spectrum in the solar wind

TL;DR

This paper investigates how linear wave processes in an inhomogeneous plasma can produce the 1/f spectrum observed in solar wind fluctuations, emphasizing the role of phase mixing and surface Alfvén waves.

Contribution

It demonstrates that linear interactions of surface Alfvén waves with inhomogeneous plasma can generate a 1/f spectrum, offering a new explanation for observed solar wind fluctuations.

Findings

Linear cascade of surface Alfvén wave energy leads to 1/f spectrum.

Inhomogeneous density spectrum influences wave energy distribution.

Linear processes can produce the observed 1/f spectral behavior.

Abstract

The origin and evolution of the 1/f power law observed in the energy spectrum of solar coronal and solar wind fluctuations at scales of around an hour is not entirely understood. Several existing theories aim at explaining it, involving both linear and nonlinear mechanisms. An often overlooked property of the solar corona and solar wind is their highly inhomogeneous nature. In this paper we investigate the linear evolution of pure Alfv\'en and surface Alfv\'en waves propagating through a plasma which is inhomogeneous across the magnetic field. The inhomogeneity is given by density, which we model to be two-dimensional colored noise, with power spectral slopes ranging from -2 to -1. Alfv\'en waves propagate independently on individual magnetic field lines, and eventually get completely out of phase through the process of phase mixing, leading to unrealistic spectra. When the coupling between the inhomogeneous background and the propagating waves is fully accounted for, transverse waves such as surface Alfv\'en waves (also referred to as kink or Alfv\'enic) appear, showing collective wave behavior of neighboring magnetic field lines with different Alfv\'en speeds. We show that the linear cascade of surface Alfv\'en wave energy, induced by phase mixing and resonant absorption, leads to a perpendicular wave energy spectrum which tends to the perpendicular power spectrum of the background density. Based on our model, we propose that a perpendicular density power spectrum of 1/f in the solar corona can induce, through linear processes, the 1/f spectrum of the fluctuations that is observed at the largest scales.