Magnetohydrodynamic Turbulence and Turbulence in the Interplanetary Medium

磁流体动力湍流和行星际介质中的湍流

• 批准号: 9713595
• 负责人: William Matthaeus
• 金额: $ 31.7万
• 依托单位: Bartol Research Institute
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1997
• 资助国家: 美国
• 起止时间: 1997-12-01 至 2002-05-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9713595&HistoricalAwards=false
• 关键词: Magnetohydrodynamic; Turbulence; Interplanetary; Medium

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.

研究者继续使用流体和磁性水力动力学（MHD）方程，以评估太阳现象中的湍流，例如扩展的太阳电晕，太阳风，磁层和星际培养基。 湍流在冠状物理学中起着至关重要的作用，导致太阳风的起源，通过高层等离子体和能量颗粒的能量转移对太空天气的介导，以及影响外层结构的能量颗粒的湍流扩散。 研究人员进一步阐明了MHD湍流的基本特性。 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值的相关分析和解释。