Magnetohydrodynamic Turbulence and Turbulence in the Interplanetary Medium

研究人员继续使用流体和磁流体动力学（MHD）方程来评估太阳现象中的湍流，如扩展的日冕，太阳风，磁层和星际介质。 湍流在日冕物理学中发挥着至关重要的作用，导致太阳风的起源、通过日光层等离子体和高能粒子的能量转移来调解空间天气，以及影响日光层外结构的高能粒子的湍流扩散。 进一步阐明了MHD湍流的基本性质。 他整合了MHD和流体模拟技术，传输理论与数值实现，湍流和粒子扩散的分析理论，以及基于航天器观测的相关分析和解释。

The investigator continues working with fluid and magnetohydrodynamic (MHD) equations to assess turbulence in solar phenomena such as the extended solar corona, solar wind, magnetosphere, and interstellar medium. Turbulence plays a critical role in coronal physics leading to the origin of the solar wind, mediation of space weather by energy transfer through the heliospheric plasma and energetic particles, and turbulent diffusion of energetic particles impacting the outer heliosphere structure. The investigator further elucidates basic properties of MHD turbulence. He integrates MHD and fluid simulation techniques, transport theory with numerical implementations, analytical theory of turbulence and particle diffusion, and related analysis and interpretation based on spacecraft observations.