SOLARNET Conference: The Many Scales of the Magnetic Sun

Spicules are one of the most intriguing phenomena of the lower solar atmosphere. From our initial work on how solar p-modes may generate spicules (Nat. 2004), through using radial MHD simulations showing the formation of a forest of them (Nat. Phys. 2022), finally we are able to report a more unified theory of spicular physics, underpinned with solar observational and laboratory experimental confirmation. Namely, bringing together SDO and IRIS observations, numerical simulations of the Sun (from convective zone to low corona) and laboratory fluid dynamics experiments we provide an insights into the mechanism underlying the ubiquity of fluid and plasma jets: how to generate a forest of spicules on the Sun.

Satellite data together with 3D rMHD simulations capture a significant rotation amongst clusters of spicules. We show how this swirly spicular motion is linked to hot rotating plasma columns – a phenomenon we label as coronal swirling conduit (CoSCo). The spicules themselves appear as folds of drapery made of dense and cool plasma, in the solar atmosphere. A particular class of tall CoSCos seen in our simulations can potentially form by feeding on spicules and channeling their energy to the upper reaches of the solar atmosphere.

Finally, we propose, how with DKIST data the next step may be made in this context.