Kelvin–Helmholtz instability and Alfvénic vortex shedding in solar eruptions
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We report on a three-dimensional MHD numerical experiment of a small-scale coronal mass ejection (CME)-like eruption propagating though a nonmagnetized solar atmosphere. We find that the Kelvin–Helmholtz instability (KHI) develops at various but specific locations at the boundary layer between the erupting field and the background atmosphere, depending on the relative angle between the velocity and magnetic field. KHI develops at the front and at two of the four sides of the eruption. KHI is suppressed at the other two sides of the eruption. We also find the development of Alfvénic vortex shedding flows at the wake of the developing CME due to the 3D geometry of the field. Forward modeling reveals that the observational detectability of the KHI in solar eruptions is confined to a narrow ≈10° range when observing off-limb, and therefore its occurrence could be underestimated due to projection effects. The new findings can have significant implications for observations, for heating, and for particle acceleration by turbulence from flow-driven instabilities associated with solar eruptions of all scales.
Syntelis , P & Antolin , P 2019 , ' Kelvin–Helmholtz instability and Alfvénic vortex shedding in solar eruptions ' , Astrophysical Journal Letters , vol. 884 , no. 1 , L4 , pp. 1-7 . https://doi.org/10.3847/2041-8213/ab44ab
Astrophysical Journal Letters
Copyright © 2019 American Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.3847/2041-8213/ab44ab
DescriptionFunding: UK STFC Ernest Rutherford Fellowship (No. ST/R004285/1) (P.A.). ERC synergy grant “The Whole Sun” (P.S.).
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