  Prominences in the solar atmosphere represent an intriguing and delicate
balance of forces and thermodynamics in an evolving magnetic topology. How this
relatively cool material comes to reside at coronal heights, and what drives
its evolution prior to, during, and after its appearance remains an area full
of open questions. We deliberately focus on the levitation-condensation
scenario, where a coronal flux rope forms and eventually demonstrates in-situ
condensations, revisiting it at extreme resolutions down to order 6 km in
scale. We perform grid-adaptive numerical simulations in a 2.5D translationally
invariant setup, where we can study the distribution of all metrics involved in
advanced magnetohydrodynamic stability theory for nested flux rope equilibria.
We quantify in particular Convective Continuum Instability (CCI), Thermal
Instability (TI), baroclinicity, and mass-slipping metrics within a series of
numerical simulations of prominences formed via levitation-condensation.
Overall, we find that the formation and evolution of prominence condensations
happens in a clearly defined sequence regardless of resolution or background
field strength between 3 and 10 Gauss. The CCI governs the slow evolution of
plasma prior to the formation of distinct condensations found to be driven by
the TI. Evolution of the condensations towards the topological dips of the
magnetic flux rope is a consequence of these condensations forming initially
outside of pressure balance with their surroundings. From the baroclinicity
distributions, smaller-scale rotational motions are inferred within forming and
evolving condensations. Upon the complete condensation of a prominence
`monolith', the slow descent of this plasma towards lower heights appears
consistent with the mass-slippage mechanism driven by episodes of both local
current diffusion and magnetic reconnection.
