太阳物理研究组知识库

大时空尺度湍流磁重联(LTSTMR)是空间物理、太阳物理、宇宙学领域中一种普遍存在的爆发现象。磁能转移-释放-耗散、等离子体加热及高能粒子加速是研究该类现象的核心内容,而研究湍流在LTSTMR中如何起作用是解决以上问题的关键所在。2D/2.5D磁重联模型因其在物理图像简化方面忽略了自然界爆发现象的3D属性和本质。文中基于新型HPIC-LBM粒子算法,在天河2号平台上开展了LTSTMR十万核心级别的数值实验工作。首次获得了太阳大气活动磁重联精细演化(0～500 km)耗散区内oblique不稳定性证据。证明了耗散区内微观集体集合效应宏观表现的3种具体形式:湍流磁场self-generating-organization、湍动等离子体self-feeding-sustaining及磁场与等离子体间的相互作用。该研究为在超算平台上应用三维磁重联模型开展大时空尺度湍流磁重联提供了一种新途径。

Large temporal-spatial scale turbulent magnetic reconnection (LTSTMR) is a general explosive astrophysical phenomena in space physics, solar physics and cosmology. To investigate this phenome, the mechanism of magnetic energy transfer-release-dissipation, plasma heating and acceleration of high energy particle should be learned, where the key is the role of trubulence. Previous 2D/2.5D simulation can only provide simplified physical pictures, which ignores the 3D nature and properties. By HPIC-LBM simulation on Tianhe-2 from National Supercomputer Center in Guang Zhou (NSCCGZ) with up to 100000 CPU cores, the existence of oblique instability was firstly proved from fine structure simulation (0～500km) of solar atmosphere activities. It also presented three kind of macroscopic representation inside the dissipation area: self-generation-organization, self-feeding-sustaining and interaction between magnetic field and plasma. This research provides a new tool for investigating 3D LTSTMR phenomenon on supercomputer.