Frequency-dependent Alfvén-wave propagation in the solar wind: Onset and suppression of parametric decay instability

Abstract

Using numerical simulations, we investigate the onset and suppression of parametric decay instability (PDI) in the solar wind, focusing on the suppression effect by the wind acceleration and expansion. We also discuss the role of PDI in generating the density fluctuation in the solar wind and the cross-helicity evolution up to $1\mathrm{au}$. Numerical simulations from the coronal base to 1 au are conducted in a self-consistent manner; we take into account the feedback of wave energy and pressure in the background. Monochromatic waves with various injection frequencies $f_0$ are injected to discuss the suppression of PDI, while broadband waves are applied to compare the numerical results with observation. We find, via the simulations with monochromatic waves, that high-frequency ($f_0\gtrsim 10^{-3}\mathrm{Hz}$) Alfvén waves are subject to PDI. Meanwhile, the maximum growth rate of the PDI of low-frequency ($f_0\lesssim 10^{-4}\mathrm{Hz}$) Alfvén waves becomes negative due to acceleration and expansion effects. Medium-frequency ($f_0\approx 10^{-3.5}\mathrm{Hz}$) Alfvén waves have a positive growth rate but do not show the signature of PDI up to 1 au because the growth rate is too small. The medium-frequency waves experience neither PDI nor reflection so they propagate through the solar wind most efficiently. This is called the frequency-filtering mechanism of the solar wind. The simulations with broadband waves indicate that the observed trend of the density fluctuation is well explained by the evolution of PDI while the observed cross-helicity evolution is in agreement with low-frequency wave propagation.

Accepted for publication in The Astrophysical Journal

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