Morphology and dynamics of solar prominences from 3D MHD simulations

TL;DR

This study uses 3D MHD simulations to explore the formation, structure, and dynamics of solar prominences, revealing how magnetic parameters influence their stability and morphology.

Contribution

It provides a detailed numerical analysis of prominence evolution, including the effects of magnetic shear and instabilities, advancing understanding of prominence behavior.

Findings

Detached and connected prominence configurations identified.

Magnetic Rayleigh-Taylor instabilities often develop, creating vertical structures.

Magnetic shear can suppress instabilities and influence prominence shape.

Abstract

In this paper we present a numerical study of the time evolution of solar prominences embedded in sheared magnetic arcades. The prominence is represented by a density enhancement in a background stratified atmosphere and is connected to the photosphere through the magnetic field. By solving the ideal magnetohydrodynamic (MHD) equations in three dimensions we study the dynamics for a range of parameters representative of real prominences. Depending on the parameters considered, we find prominences that are suspended above the photosphere, i.e., detached prominences, but also configurations resembling curtain or hedgerow prominences whose material continuously connects to the photosphere. The plasma$-\beta$ is an important parameter that determines the shape of the structure. In many cases magnetic Rayleigh-Taylor (MRT) instabilities and oscillatory phenomena develop. Fingers and plumes are generated, affecting the whole prominence body and producing vertical structures in an essentially horizontal magnetic field. However, magnetic shear is able to reduce or even to suppress this instability.