A Method for Determining the Locations and Configurations of Magnetic Reconnection within 3D Turbulent Plasmas
arXiv:2312.15589 · doi:10.1051/0004-6361/202347564
Abstract
Context. Three-dimensional (3D) reconnection is an important mechanism for efficiently releasing energy during astrophysical eruptive events, which is difficult to be quantitatively analyzed especially within turbulent plasmas. Aims. In this paper, an efficient method for identifying locations and configurations of 3D reconnection from MHD data is developed. Methods. This method analyzes the local nonideal electric field and magnetic structure at an arbitrary position. As only performing algebraical manipulations on the discrete field data and avoiding computationally expensive operations like field-line tracing and root-finding, this method naturally possesses high efficiency. To validate this method, we apply it to the 3D data from a high-resolution simulation of a Harris-sheet reconnection and a data-driven simulation of a coronal flux rope eruption. Results. It is shown that this method can precisely identify the local structures of discrete magnetic field. Through the information of nonideal electric field and the geometric attributes of magnetic field, the local structures of reconnection sites can be effectively and comprehensively determined. For fine turbulent processes, both qualitative pictures and quantitative statistical properties of small-scale reconnection structures can be obtained. For large-scale solar simulations, macro-scale magnetic structures such as flux ropes and eruption current sheets can also be recognized. Conclusions. We develop a powerful method to analyze multi-scale structures of 3D reconnection. It can be applied not only in MHD simulations but also in kinetic simulations, plasma experiments, and in-situ observations.
19 pages, 14 figures, 4 tables. Accepted for publication in Astronomy & Astrophysics. The code URL: https://github.com/RainthunderWYL/LoRD
References in corpus (16)
- The Athena++ Adaptive Mesh Refinement Framework: Design and Magnetohydrodynamic Solvers
- Generalized Squashing Factors for Covariant Description of Magnetic Connectivity in the Solar Corona
- Magnetic reconnection in the era of exascale computing and multiscale experiments
- A trilinear method for finding null points in a 3D vector space
- Current sheet formation and non-ideal behaviour at three-dimensional magnetic null points
- Reconnection-Driven Energy Cascade in Magnetohydrodynamic Turbulence
- Ion and Electron Acceleration in Fully Kinetic Plasma Turbulence
- Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
- FastQSL: A Fast Computation Method for Quasi-separatrix Layers
- Three-dimensional Turbulent Reconnection within Solar Flare Current Sheet
- Identification of active magnetic reconnection using magnetic flux transport in plasma turbulence
- Annihilation of Magnetic Islands at the Top of Solar Flare Loops
- Formation and Evolution of Coherent Structures in 3D Strongly Turbulent Magnetized Plasmas
- Grow-up of a Filament Channel by Intermittent Small-scale Magnetic Reconnection
- Extended magnetic reconnection in kinetic plasma turbulence
- A comparison of methods for finding magnetic nulls in simulations and in situ observations of space plasmas