Plasma Vortices on the Sun Captured for the First Time

Plasma vortices on the sun have been photographed clearly enough, for the first time, to pin down where they come from. A team from the US National Solar Observatory, the German Max Planck Institute for Solar System Research and the US High Altitude Observatory reported in the journal Nature that it had identified a Kelvin Helmholtz instability on the sun’s visible surface, a phenomenon theory had predicted for decades but no instrument had managed to record. The observatory’s announcement went out on August 5, 2026, the study’s lead author is David Kuridze, and the paper is filed under DOI 10.1038/s41586-026-10871-3.

The images were taken by the Daniel K. Inouye Solar Telescope, sited near the summit of Haleakala on Maui, Hawaii. A 4 meter mirror makes it the largest solar telescope in the world. The instrument delivered its first images of the sun’s surface in early 2020, already the most detailed ever taken at the time, but this result required going a step further: resolving features roughly twenty kilometers across on a body some 150 million kilometers away.

To detect the vortices, we had to resolve structures on the sun’s surface that were about 20 kilometers in size.

Said Michiel van Noort, a scientist at the Max Planck Institute who worked on the observations and on processing and restoring the images. The wide-band imaging camera used for the observations also comes from that institute.

Where the vortices form

Not just anywhere. They form along the edges of granules, cells of churning plasma that densely cover the sun’s visible surface. Granulation behaves like a boiling liquid: hot plasma rises from below, cools near the top and sinks back down. A single granule spans between 500 and 2,000 kilometers, which makes a twenty kilometer structure at its edge up to a hundred times smaller than the cell itself. Along those edges, neighboring layers of plasma move at different speeds, the condition an instability needs in order to appear at all.

The Kelvin Helmholtz instability itself arises when two fluids slide past each other at different speeds and generate shear at their boundary. Small disturbances along that boundary grow into waves and spirals that resemble an ocean wave about to break. Lord Kelvin and Hermann von Helmholtz first described the phenomenon around 1870, and since then it has turned up across fluid dynamics, meteorology, oceanography and astrophysics, from waves on a lake and cloud formations to the atmospheres of Jupiter and Saturn and the contact between the solar wind and planetary magnetospheres. On the sun, it had been missing, even though it was expected there.

The image and the simulation agree

The image alone was not enough for the conclusion. The team compared its observations against numerical simulations of the photosphere, run with code maintained by HAO and MPS. Dozens of vortex structures appeared along the edges of magnetic regions in both the images and the simulations, behaving in strikingly similar ways. The spacing between individual vortices, what physicists call the instability’s wavelength, came out between 50 and 65 kilometers in both cases. It was that match that made the identification possible.

We believe that the discovery of the Kelvin Helmholtz instability in the solar photosphere, supported by analysis of numerical simulations, is a major step forward in our understanding of the dynamics and evolution of solar and stellar plasma, and that it will serve as a foundation for future discoveries.

That is how David Boboltz, deputy director of the National Solar Observatory, described the finding.

Why is the corona hotter than the surface below it?

The sun’s outer atmosphere is heated to roughly one million degrees Kelvin, even though the surface beneath it is far cooler. It is one of the oldest open questions in solar physics, and the vortices could be part of the answer. They occur constantly, wherever the magnetic field is strong enough, so they could act as a continuous engine twisting magnetic field lines. A twisted field stores free magnetic energy, and its sudden release drives everything from the smallest nanoflares to major eruptions, jets and coronal mass ejections, the very events that disrupt satellites, power grids and navigation on Earth.

The Kelvin Helmholtz instability is likely a mechanism that contributes to heating the outer atmosphere, and is part of the solution to the long standing puzzle of why stars have coronas heated to a million degrees Kelvin.

Said Thomas Rimmele, chief technologist at the National Solar Observatory. His colleague Friedrich Woeger, a senior scientist at the same institution, set the boundary more cautiously.

We are only beginning to recognize the far reaching impact the discovery of the Kelvin Helmholtz instability has on our understanding of the link between the motion of magnetized plasma and the transport and release of energy in the sun’s upper atmosphere.

There is another side to the finding, less visible but perhaps more far reaching. The vortices efficiently mix magnetized and non magnetized plasma at the surface, which speeds up the dispersal of magnetic field through the sun’s atmosphere. The solar cycle lasts about eleven years, fast by cosmic standards, and existing models have struggled to explain how magnetic flux disappears that quickly. The missing dispersal mechanism may be found here.

What the study does not show

It does not show how much energy the vortices actually carry upward. That figure has not been measured, it is the subject of the next phase of analysis, which plans to automate vortex detection in the data. The link to coronal heating is still framed as the contribution of one mechanism, not as an explanation of the phenomenon, and the authors themselves describe it that way.

The identification, further, rests on the match between observation and simulation, and a simulation is not an independent measurement but a model built on assumed equations. The match in detail is a strong argument, but it remains an argument from agreement. A twenty kilometer structure, finally, sits right at the edge of what the world’s largest solar telescope can currently resolve, so confirmation from another instrument has yet to arrive.