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数值模型研究快速太阳风的湍流生成，该模型求解质子扩散和共振波增长的耦合准线性方程。在本项目期间，主要研究者（PI）将逐步向数值模型中添加更多的物理过程，并最终将模拟输出与观测结果进行比较。在每一步中，研究小组都将探索扩大他们的模型对日冕洞质子和次要离子的加热和加速的影响。PI声称，这些研究将导致更详细的日冕中太阳风生成的动力学模型，从而能够更好地理解和预测日光层环境的状态。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。具体而言，该团队将在他们的模拟中添加非线性波效应，如共振加宽和湍流传输，以产生太阳风中真实的Alfvén波增长。他们还将把这种非线性计算纳入他们的非均匀冕洞模型。该团队计划构建一个详细的动力学模型，用于不平衡波场加热的冕洞质子的径向演化，获得动力学粒子和波态的预测。PI还将把他的模型输出与现有航天器仪器拍摄的实际日冕洞观测结果进行比较。建模工作将产生粒子和波通量的预测，这些预测将指导未来NASA航天器任务的开发，并由未来的NASA航天器任务进行测试，例如“太阳轨道器”和“太阳探测器+”。这些任务将在新罕布什尔州大学的理论湍流和重连小组内执行，这将为研究生和博士后研究人员提供参与该项目的机会。