Solar Magnetic Field Braids May Have a Previously Hidden Cause

Scientists using the Daniel K. Inouye Solar Telescope (DKIST) in Hawai'i have found a mechanism called the Kelvin-Helmholtz Instability (KHI) that may explain how the Sun's outer atmosphere is heated. The KHI occurs when fluids move at different velocities, creating vortices that destabilize magnetic fields. This process is linked to "flux braiding," where magnetic fields twist and snap, releasing energy that heats the corona. The discovery may also explain similar phenomena on other stars.

The study shows that the Sun's surface has dozens of vortex-like structures along the edges of magnetic regions, which align with KHI occurrences. These vortices are formed by the motion of neighboring layers of solar plasma, creating conditions for the instability. The KHI is a well-studied phenomenon, and the DKIST images confirm its presence in the solar photosphere. The simulations and observations show a clear correlation between KHI and the formation of magnetic field braids.

The KHI is a constant process on the Sun, contributing to the heating of the corona and mixing of magnetized and non-magnetized plasma. The study highlights how the DKIST provides the highest-resolution data to validate solar magnetohydrodynamic simulations. The findings suggest that the KHI is a hidden but essential process that maintains the Sun's dynamic atmosphere. The discovery may help solve the long-standing question of why the corona is so hot, and it offers new insights into solar physics and space weather.

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