Investigation of the anisotropic characteristics in the flare loop turbulence magnetic reconnection through improved RHPIC-LBM on the supercomputer platform

The sources and origins of solar energetic particles (SEPs), especially for the GeV-level events, are the premise and fundamental issue for SEP-induced space-weather disasters. Observational evidence indicates that the anisotropy properties exist in the 3D large temporal-spatial turbulence magnetic reconnection(3D LTSTMR) in solar activities, which is essential to understanding the energy conversion between magnetic energy and acceleration energy (bulk kinetic energy) and heating energy (thermal kinetic energy) over different particle species (e.g., electron, ion, 3He/4He, and other heavier particles), and SEPs characteristics and acceleration propagation in non-ideal diffusion regions. In this work, on the supercomputer platform (GPU heterogeneous architecture & ARM architecture), a 3D spherical coordinates system () for flare loop 3D LTSTMR is applied to explore the helical turbulence-induced anisotropic characteristics (TAC, including turbulence anisotropy, TA; turbulence intensity, TI; and spectral anisotropy properties) through the improved relativistic hybrid particle-in-cell and lattice Boltzmann (RHPIC-LBM2) code. Firstly, we deduced the explicit expression of the turbulence-induced dissipation-diffusion (TIDD) terms under fully coupled hydro-dynamic-kinetic continuous scales by considering the turbulence-resistance-induced self-generated organization and the turbulence-viscosity-induced self-feeding-sustaining with filter theory. Then, we improved the input module and dissipation-diffusion module and added a new TIDD module in the original RHPIC-LBM model algorithm code. Finally, we analyze the TAC in the impulsive twisted multi-magnetic flux ropes (MFLs) & multi-current plasma flux ropes (CFLs) & multi-plasma flux ropes (PFLs). It is found that the magnetic strength (MFLs), current density (CFLs), and charged flow (PFLs, electron, ion, 3He/4He) anisotropy exist and vary in different evolution times (65.6000s to 74.3467s) in the different direction ( plane,  plane), in the different scale (R=24Mm) at B&U decoupled frozen-in condition broken region. The main findings of the present study are as follows: 1) The TAC in the radial direction is stronger than in the azimuthal direction ( plane) and in the polar direction ( plane); 2) The TAC of magnetic strength (MFLs), current density (CFLs), and charged flow (PFLs) do not overlap in the evolution process; 3) The TAC increases with the evolution time and reaches its maximum when the turbulence enters the fully developed stage; 4) The TAC decreases with the decreasing scale and exhibits weakness when entering the micro-kinetic scale. We anticipate these results to be a key point and give new insights for evaluation of the short-time real-time extremely GeV-SEPs prediction (GPU heterogeneous architecture) and the real-time long-time SEP monitor (ARM architecture), which serve for the 'China Science Development Strategy: Space Science (2020-2035)', and 'The Strategic Position of Space Astronomy: China's Space Science 2035 Development Strategy' in NSFC&CAS. and 'National Mid- and Long-term Plan for Space Science in China (2024-2050). 

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