Magnetohydrodynamic Turbulence, Charged Particle Transport, and Turbulence in the Extended Solar Atmosphere

磁流体动力湍流、带电粒子输运以及扩展太阳大气中的湍流

• 批准号: 0539995
• 负责人: William Matthaeus
• 金额: $ 45万
• 依托单位: University of Delaware
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2005
• 资助国家: 美国
• 起止时间: 2005-12-15 至 2010-11-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0539995&HistoricalAwards=false
• 关键词: Magnetohydrodynamic; Turbulence; Charged; Particle; Transport

Turbulence is a complex nonlinear dynamical behavior that we can observe in space plasmas over a wide range of temporal and spatial scales. This proposal offers to advance our understanding of plasma turbulence, a feature of nonlinear plasma electrodynamics that pervades and shapes basic physical phenomena throughout much of the universe. Much of the nonthermal energy stored by space and astrophysical plasmas is found in structures or fluctuations that are well described by magnetohydrodynamic (MHD) models. The solar corona, the solar wind, the magnetosphere, and the interstellar medium may exhibit MHD turbulence, ranging from the largest scales down to the scales at which kinetic dissipation becomes strong. Understanding this MHD turbulence is critical to problems related to coronal heating, the acceleration of the solar wind, distributed heating of the solar wind, mediation of "space weather" by transfer of energy through the heliosphere, and the transport of solar and galactic energetic charged particles throughout the solar system. This proposal continues highly productive projects previously funded by the NSF. The PI intends to further elucidate basic properties of MHD turbulence and transport theories for macroscopic or inhomogeneous processes that include turbulence at smaller scales. He will use test particle theory and simulation to study energetic particle response to turbulence, and adopt an integrated approach using MHD and fluid simulation techniques, transport theory, analytical theories of turbulence and particle diffusion, and related analysis and interpretation of spacecraft observations. In this effort, the PI includes an educational component, supervision and mentorship of junior personnel, and potential contributions to analysis techniques, computational methods, and parallel computing strategies, as well as to industrial and cross disciplinary methodologies and applications.

湍流是一种复杂的非线性动力学行为，我们可以在各种时间和空间尺度上观察到空间等离子体。该建议旨在提高我们对等离子体湍流的理解，这是非线性血浆电动力学的特征，该特征遍及整个宇宙的大部分地区基本的物理现象。空间和天体物理等离子体存储的许多非热能都在通过磁性水力动力学（MHD）模型很好地描述的结构或波动中发现。太阳电晕，太阳风，磁层和星际介质可能表现出MHD湍流，从最大的尺度到动力学耗散变得强大的尺度。了解这种MHD湍流对于与冠状，太阳风的加速度，太阳风的加速相关的问题至关重要，太阳风的分布加热，通过在整个太阳能系统中通过热球传递通过热层传递的“太空天气”以及太阳能和银河系充电颗粒的传输。 该提案继续以前由NSF资助。 PI旨在进一步阐明MHD湍流的基本特性和用于宏观或不均匀过程的理论，包括较小尺度的湍流。他将使用测试粒子理论和仿真来研究对湍流的能量粒子反应，并使用MHD和流体模拟技术，传输理论，湍流和粒子扩散的分析理论以及航天器观测的相关分析和解释。在这项工作中，PI包括对初级人员的教育组成部分，监督和指导，以及对分析技术，计算方法以及并行计算策略的潜在贡献，以及工业和跨学科方法和应用。