A unified model of solar prominence formation
C. J. Huang, J. H. Guo, Y. W. Ni, A. A. Xu, P. F. Chen

TL;DR
This paper presents a unified model of solar prominence formation by demonstrating that both direct injection and evaporation-condensation mechanisms are manifestations of localized chromospheric heating, confirmed through radiative hydrodynamic simulations.
Contribution
The study unifies two main prominence formation models into a single framework based on the location of chromospheric heating, supported by simulation results.
Findings
Both formation mechanisms can occur under different heating locations.
A case with simultaneous injection and condensation processes was identified.
Simulations confirm the unified model's validity.
Abstract
Several mechanisms have been proposed to account for the formation of solar prominences or filaments, among which direct injection and evaporation-condensation models are the two most popular ones. In the direct injection model, cold plasma is ejected from the chromosphere into the corona along magnetic field lines; In the evaporation-condensation model, the cold chromospheric plasma is heated to over a million degrees and is evaporated into the corona, where the accumulated plasma finally reaches thermal instability or non-equilibrium so as to condensate to cold prominences. In this paper, we try to unify the two mechanisms: The essence of filament formation is the localized heating in the chromosphere. If the heating happens in the lower chromosphere, the enhanced gas pressure pushes the cold plasma in the upper chromosphere to move up to the corona, such a process is manifested as…
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