First Direct Imaging of a Kelvin–Helmholtz Instability by PSP/WISPR

• Published in: The Astrophysical journal 2024-04, Vol.964 (2), p.139
• Main Authors: Paouris, Evangelos, Stenborg, Guillermo, Linton, Mark G., Vourlidas, Angelos, Howard, Russell A., Raouafi, Nour E.
• Format: Article
• Language: English
• Subjects: Boundary layers; Corona; Coronal mass ejection; Eddies; Heliosphere; Instability; Kelvin-Helmholtz instability; Magnetic fields; Magnetic properties; Solar corona; Solar coronal mass ejections; Solar probes; Solar wind; Stability analysis; The Sun; Thickness measurement; Topology; White light
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad2208

We present a comprehensive analysis aimed at proving the hypothesis that a train of small-scale features observed by the Wide-field Imager (WISPR) onboard the Parker Solar Probe (PSP) are the signature of a Kelvin–Helmholtz instability (KHI). These features were seen near the flank of a Coronal Mass Ejection (CME) wake between 7.5 R ⊙ and 9.5 R ⊙ , lasting for about 30 minutes. The CME was a slow event, associated with a streamer blowout. We analyzed the size of the eddies and found growth during their evolution while maintaining separation distances and alignment typical of Kelvin–Helmholtz vortexes. We then assessed the magnetic field conditions that would make the observation of such an instability plausible. Two methods were used to cross-check our findings. The measured thickness of the boundary layer supports KHI candidacy, and the estimated linear growth rate suggests nonlinear saturation within the expected timescale. We conclude that a KHI is a plausible explanation for the observed features, and therefore that such instabilities might exist in the low and middle solar corona (within ∼15 R ⊙ ) and can be detected in white light observations. Their observation, however, might be rare due to stringent conditions like the observer’s proximity, suitable viewing circumstances, magnetic field topology, and flow properties. This study highlights the unique capability of PSP/WISPR in observing such phenomena, especially as PSP perihelia reach closer distances to the Sun.