Parametric decay and the origin of the low frequency Alfvénic spectrum of the solar wind

Abstract

The fast solar wind shows a wide spectrum of transverse magnetic and velocity field perturbations. These perturbations are strongly correlated in the sense of Alfvén waves propagating mostly outward, from the Sun to the interplanetary medium. They are likely to be fundamental to the acceleration and the heating of the solar wind. However, the precise origin of the broadband spectrum is to date unknown. Typical periods of chromospheric Alfvén waves are limited to a few minutes, and any longer period perturbations should be strongly reflected at the transition region. In this work, we show that minute long Alfvénic fluctuations are unstable to the parametric instability. Parametric instability enables an inverse energy cascade by exciting several hours long periods Alfvénic fluctuations together with strong density fluctuations (typically between 1 and $20R_{\odot }$). These results may improve our understanding of the origin of the solar wind turbulent spectrum and will be tested by the Parker Solar Probe.

arXiv comment11 pages, 11 figures, to appear in the Astrophysical Journal

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• Flux-tube-dependent propagation of Alfvén waves in the solar corona
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