Numerical Modeling of Prominences and Coronal Rain with the MPI-AMRVAC Code

TL;DR

MPI-AMRVAC enables versatile, high-resolution simulations of solar prominences and coronal rain across HD, MHD, and magneto-frictional regimes. The review assesses 1D to 3D studies of magnetic-field structures (flux ropes, dips), thermodynamic condensation processes (evaporation-condensation and levitation-condensation), and dynamic phenomena (oscillations, counterstreaming, Rayleigh–Taylor instabilities), linking simulations to observations through synthetic diagnostics. It highlights how heating, conduction, radiation, and magnetic topology govern condensation formation, thread morphology, and mass cycling, with 3D models clarifying the prominence–corona mass exchange and the alignment of threads with magnetic structures. By detailing forward-modeling approaches from approximate emissivity to NLTE radiative transfer (Lightweaver/Promweaver, DexRT), the work demonstrates how simulations can be meaningfully compared to EUV and H$\alpha$ observations, guiding future development toward fully coupled 3D radiative-MHD and partially ionized plasmas.

Abstract

This review surveys recent advances in the numerical modeling of solar prominences and coronal rain achieved with the fully open-source adaptive-grid, parallelized Adaptive Mesh Refinement Versatile Advection Code (MPI-AMRVAC). We examine how these models have contributed to our understanding of the formation and evolution of cool plasma structures in the solar corona. We first discuss prominence models that focus on prominence formation and their dynamic behavior. We then turn to coronal rain, highlighting its connection to thermal instability and its role in the exchange of mass and energy between the corona and chromosphere. Particular attention is given to the growing efforts to connect simulations with observations through synthetic emission and spectral diagnostics.

Figures (58)

• Figure 1: Side (left) and top (right) views of the flux rope at time $0.0$ and $114.5$ minutes. The bottom magnetograms are shown in gray with the polarity-inversion line plotted in white. Magnetic field lines are colored by the local current density $J_x$ in the rainbow color table. The vertical planes are colored by number density in the blue-red color table. Adapted from Xia:2014apj. © AAS. Reproduced with permission.
• Figure 2: (a) Twisting and (b) converging velocity fields (indicated by arrows) applied at the footpoints, overlaid on the bottom boundary magnetogram shown in grayscale. Adapted from Xia:2014apj. © AAS. Reproduced with permission.
• Figure 3: Two models applying the supergranular motions and with or without Coriolis force at times 15, 45, and 60. In panels a–f, magnetic field lines are shown in rainbow colors, and the polarity-inversion line in cyan. The photosphere is colored by a radial magnetic field saturated at $\pm20$ G. Zoom-in views are shown in panels g and h, where gray arrows present the photospheric horizontal velocity field. Adapted from Liu:2022apjl.
• Figure 4: (a) Magnetic flux rope (MFR) constructed by the MFR embedding method, further relaxed by the MF method, overlaid on the 304 Å image, which was observed by STEREO-A/EUVI at 01:11 UT on 2011 June 21. The viewing angle is from STEREO-A. (b) Same as (a) but viewed from SDO. (c) Same as (a) but viewed from STEREO-B. Adapted from Guo:2019apjl. © AAS. Reproduced with permission.
• Figure 5: (a) Magnetic dips computed from the MFR constructed by the MFR embedding method, further relaxed by the MF method, overlaid on the 304 Å image, which was observed by STEREO-A/EUVI at 01:11 UT on 2011 June 21. The viewing angle is from STEREO-A. (b) Same as (a) but viewed from SDO. (c) Same as (a) but viewed from STEREO-B. Adapted from Guo:2019apjl. © AAS. Reproduced with permission.