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Aims. We begin by exploring the influence of two classes of commonly adoptedheating models on the formation behaviour of solar prominences. These modelsconsider either an exponential variation dependent on height alone, or localdensity and magnetic field conditions. We highlight and address some of thelimitations inherent to these early approximations by proposing a new, dynamic2D flux rope heating model that qualitatively accounts for the 3D topology ofthe twisted flux rope field. Methods. We performed 2.5D grid-adaptive numericalsimulations of prominence formation via the levitation-condensation mechanism.A linear force-free arcade is subjected to shearing and converging motions,leading to the formation of a flux rope containing material that may succumb tothermal instability. The eventual formation and subsequent evolution ofprominence condensations was then quantified as a function of the specificbackground heating prescription adopted. For the simulations that consider thetopology of the flux rope, reduced heating was considered within a dynamicallyevolving ellipse that traces the flux rope cross-section. This ellipse iscentred on the flux rope axis and tracked during runtime using an approachbased on the instantaneous magnetic field curvature. Results. We find that thenature of the heating model is clearly imprinted on the evolution andmorphology of any resulting prominences: one large, low-altitude condensationis obtained for the heating model based on local parameters, while theexponential model leads to the additional formation of smaller blobs throughoutthe flux rope which then relocate as they tend towards achieving hydrostaticequilibrium. Finally, a study of the condensation process in phase spacereveals a non-isobaric evolution with an eventual recovery of uniform pressurebalance along flux surfaces.

The influence of flux rope heating models on solar prominence formation