SHINE: Kinetic Heating of Coronal Hole Ions for Generation of the Solar Wind by Imbalanced Turbulence

SHINE：冕洞离子的动力学加热，通过不平衡湍流产生太阳风

• 批准号: 0962506
• 负责人: Philip Isenberg
• 金额: $ 43.41万
• 依托单位: University of New Hampshire
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2010
• 资助国家: 美国
• 起止时间: 2010-03-01 至 2014-02-28
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0962506&HistoricalAwards=false
• 关键词: SHINE; Kinetic; Heating; Coronal; Hole

The project will investigate the turbulent generation of the fast solar wind by using an existing numerical model that solves the coupled quasilinear equations of proton diffusion and resonant wave growth. During this project, the Principal Investigator (PI) will progressively add more physical processes to the numerical model and finally compare the simulation output with observations. At each step, the team will explore the consequences of expanding their model on the heating and acceleration of coronal hole protons and minor ions. The PI asserts that these investigations will lead to more detailed kinetic models of the generation of the solar wind in the corona, enabling improved understanding and predictions of the state of the heliospheric environment. This work will also provide new insights into self-consistent plasma kinetics and the dissipation of plasma turbulence.Specifically, the team will add nonlinear wave effects, such as resonance broadening and turbulent transport, to their simulations in order to yield realistic Alfvén wave growth in the solar wind. They will also incorporate such nonlinear calculations into their inhomogeneous coronal hole model. The team plans to construct a detailed kinetic model for the radial evolution of coronal hole protons as heated by imbalanced wave fields, obtaining predictions for the kinetic particle and wave states. The PI will also compare his model's output with actual coronal hole observations taken by existing spacecraft instruments. The modeling effort will yield predictions of particle and wave fluxes that will guide the development of, and be tested by, future NASA spacecraft missions, such as 'Solar Orbiter' and 'Solar Probe Plus.' The tasks will be performed within the theoretical turbulence and reconnection group at the University of New Hampshire, which will provide opportunities for graduate students and postdoctoral researchers to participate in this project.

该项目将利用现有的求解质子扩散和共振波增长耦合拟线性方程的数值模型来研究快速太阳风的湍流产生。在这个项目中，首席研究员（PI）将逐步在数值模型中加入更多的物理过程，并最终将模拟输出与观测结果进行比较。在每一步中，研究小组将探索扩展他们的模型对日冕洞质子和小离子的加热和加速的影响。PI断言，这些调查将导致日冕中太阳风产生的更详细的动力学模型，从而提高对日球层环境状态的理解和预测。这项工作还将为自洽等离子体动力学和等离子体湍流耗散提供新的见解。具体来说，研究小组将在他们的模拟中加入非线性波效应，如共振展宽和湍流输运，以便在太阳风中产生真实的alfvsamn波增长。他们还将把这种非线性计算纳入他们的非均匀日冕洞模型中。该团队计划为日冕洞质子在不平衡波场加热下的径向演化建立一个详细的动力学模型，以获得粒子和波的动力学状态的预测。PI还将把他的模型输出与现有航天器仪器实际观测到的日冕洞进行比较。建模工作将产生粒子和波通量的预测，这将指导未来NASA航天器任务的发展，并由其进行测试，如“太阳轨道器”和“太阳探测器Plus”。这些任务将在新罕布什尔大学的理论湍流和重连接小组内进行，该小组将为研究生和博士后研究人员提供参与该项目的机会。