tokens: of prominence evolution involving B oriented across the 2.5D plane, or in full 3D (e.g., Hillier et al. 2012a , b ; Terradas et al. 2015 ; Keppens et al. 2015 ; Kaneko Yokoyama 2018 ; Popescu Braileanu et al. 2021 ). Nevertheless, we expect the misalignments between the pressure and density gradients to be present in 2.5D and therein induce motions inline with the RTI but on scales of the order of a flux tube. Evolution of the plasma in this way may also be characterised using baroclinicity, a component of the evolving vorticity ω that arises in a flow with anisotropic temperature, This baroclinicity considers that a misalignment between the pressure and density gradients gives rise to the rotation of plasma as it slides down a constant-pressure gradient. In general, plasma unstable to the RTI in a direction other than vertical may be identified using this approach. The fourth row of Fig. 3 details the evolution of the baroclinicity within the condensing material. At t = 7264.6 s, the signature of baroclinicity covers a broad region but one that is focussed at the periphery of the condensation region and forms a ‘U’ shape. As the evolution progresses, this ‘U’ shape is amplified in magnitude, but also becomes flat and increasingly localised to the bottom of the forming monolithic structure. In the density panels, at t = 7436.2 s we see that the two early condensations develop a curvature as they move towards the concave-up portions of the field topology. This is consistent with the baroclinicity-induced rotation. It is important to emphasise here that vorticity maps quantify, generally, the rotation of the velocity field (induced by some physical process), whereas the baroclinicity maps show the source of vorticity and represent a physical process in itself. Hence, maps of the vorticity would likely also show this rotation but would not offer information on the driving process. 3.1.3. Evolution of the monolithic prominence Figure 5 details the evolution of the now-formed prominence after the initial condensation period. Initially, between 7607.8 t 8294.2 s, it can be seen that the condensation region significantly deforms the field topology of the host flux rope as the concentration of highest density falls from an altitude of ≈9–6 Mm with an average velocity of 5 km s −1 . The largest magnetic field strength is recorded within the condensation at this time, with a value of ≈4.2 G. The falling material drags the associated field lines down and those field lines that lie directly below the condensation are compressed. Shortly after t = 8294.2 s, reconnection is triggered just above the densest portion of the falling monolith, creating a magnetically isolated region of high density that continues to fall, now with a velocity of ≈10 km s −1 . Behind this falling ‘plasmoid’ 3 , another high-density region forms in its wake, and at t ≈ 8500 s reconnection is again triggered behind this new region. Once the new density enhancement is isolated
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