Detalles de publicación
PP 024052
From eruption to post-flare rain: A 2.5D MHD model
Instituto de Astrof\'{i}sica de Canarias, 38205 La Laguna, Tenerife, Spain.
Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain.
Centre for mathematical Plasma-Astrophysics, Celestijnenlaan 200B, 3001 Leuven, KU Leuven, Belgium.
Rosseland Centre for Solar Physics, University of Oslo, Postboks 1029 Blindern, 0315 Oslo, Norway.
Institute of Theoretical Astrophysics, University of Oslo, Postboks 1029 Blindern, 0315 Oslo, Norway.
Erupting magnetic flux ropes play an important role in producing solar flares, whereas fine-scale condensed coronal rain is often found in post-flare loops. However, the formation of the MFRs in the pre-flare stage and how this leads to coronal rain in a post-eruption magnetic loop is not fully understood.
We explore the formation and eruption of MFRs, followed by the appearance of coronal rain in the post-flare loops to understand the magnetic and thermodynamic properties of eruptive events and their multi-thermal aspects in the solar atmosphere.
We performed a resistive-magnetohydrodynamic (MHD) simulation with the open-source code \texttt{MPI-AMRVAC} to explore the evolution of sheared magnetic arcades that can lead to flux rope eruptions. The system was in mechanical imbalance at the initial state and evolved self-consistently in a nonadiabatic atmosphere under the influence of radiative losses, thermal conduction, and background heating. We used an additional level of adaptive mesh refinement to achieve the smallest cell size of $\approx 32.7$ km in each direction to reveal the fine structures in the system.
The system achieves a semi-equilibrium state after a short transient evolution from its initial mechanically imbalanced condition. A series of erupting MFRs is formed due to spontaneous magnetic reconnection across current sheets that are created underneath the erupting flux ropes. A gradual development of thermal imbalance is noted at a loop top in the post-eruption phase, which leads to catastrophic cooling and to the formation of condensations. We obtain plasma blobs that fall down along the magnetic loop in the form of coronal rain. The dynamical and thermodynamic properties of these cool condensations agree well with observations of post-flare coronal rain.
We explore the formation and eruption of MFRs, followed by the appearance of coronal rain in the post-flare loops to understand the magnetic and thermodynamic properties of eruptive events and their multi-thermal aspects in the solar atmosphere.
We performed a resistive-magnetohydrodynamic (MHD) simulation with the open-source code \texttt{MPI-AMRVAC} to explore the evolution of sheared magnetic arcades that can lead to flux rope eruptions. The system was in mechanical imbalance at the initial state and evolved self-consistently in a nonadiabatic atmosphere under the influence of radiative losses, thermal conduction, and background heating. We used an additional level of adaptive mesh refinement to achieve the smallest cell size of $\approx 32.7$ km in each direction to reveal the fine structures in the system.
The system achieves a semi-equilibrium state after a short transient evolution from its initial mechanically imbalanced condition. A series of erupting MFRs is formed due to spontaneous magnetic reconnection across current sheets that are created underneath the erupting flux ropes. A gradual development of thermal imbalance is noted at a loop top in the post-eruption phase, which leads to catastrophic cooling and to the formation of condensations. We obtain plasma blobs that fall down along the magnetic loop in the form of coronal rain. The dynamical and thermodynamic properties of these cool condensations agree well with observations of post-flare coronal rain.