The influence of flux rope heating models on solar prominence formation

Context. Prominences are cool, dense clouds suspended within the solar corona. Their in situ formation through levitation-condensation mechanism is a textbook example of thermal instability, where slight energy imbalance leads to runaway process resulting condensed filamentary structures embedded concave-up portions flux rope. The detailed interplay between local radiative losses and global heating corona investigated here for prominence-forming rope structures. Aims. We begin by exploring influence two classes commonly adopted models on behaviour prominences. These consider either an exponential variation dependent height alone, or density magnetic field conditions. highlight address some limitations inherent these early approximations proposing new, dynamic 2D model that qualitatively accounts 3D topology twisted field. Methods. performed 2.5D grid-adaptive numerical simulations prominence via mechanism. A linear force-free arcade subjected shearing converging motions, leading containing material may succumb instability. eventual subsequent evolution condensations was then quantified as function specific background prescription adopted. For rope, reduced considered dynamically evolving ellipse traces cross-section. This centred axis tracked during runtime using approach based instantaneous curvature. Results. find nature clearly imprinted morphology any prominences: one large, low-altitude condensation obtained parameters, while additional smaller blobs throughout which relocate they tend towards achieving hydrostatic equilibrium. Finally, study phase space reveals non-isobaric with recovery uniform pressure balance along surfaces.