NSWP: Kinetic Turbulence-Driven Solar Wind Model Through the Resonant Cyclotron Interaction - Protons and Alpha Particles

NSWP：通过共振回旋加速器相互作用的动力学湍流驱动的太阳风模型 - 质子和阿尔法粒子

• 批准号: 0719738
• 负责人: Philip Isenberg
• 金额: $ 46.43万
• 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: 2007
• 资助国家: 美国
• 起止时间: 2007-08-01 至 2011-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0719738&HistoricalAwards=false
• 关键词: NSWP; Kinetic; Turbulence; Driven; Solar

The PI and his team will construct a detailed physics-based model of the kinetic heating and acceleration of all coronal hole ion species caused by the resonant cyclotron interaction. They will first investigate a more realistic interaction for protons, considering a broad distribution of wave propagation directions, as implied by observations and as predicted by their prior work in compressible MHD turbulence. The team will incorporate this proton heating effect into the spatial evolution of plasma flowing outward through a coronal hole, and they will then determine detailed wave intensities and spectra required to generate the observed solar wind distributions. Since the spectra of alpha particles and the dispersion relation of the waves will evolve together and affect each other, the PI will use hybrid simulations to model this behavior in a self-consistent manner. The simulation will follow these microphysical dispersive interactions, which will then be incorporated into global coronal hole equations to describe the macrophysical evolution of the solar wind with increasing radial position. The PI's team will use the kinetic description resulting from this effort to explore the limits on the resonant wave spectra and spectral energy transport rates required to yield the observed fast solar wind, as well as the response of the flow properties to changing coronal hole conditions. The PI will also apply this approach to the collisionless slow solar wind. Such rigorous kinetic understanding of the microphysical processes taking place in the coronal plasma will allow the PI's team to correctly reproduce the thermal behavior of the disturbed solar wind in global simulations of CME propagation. This knowledge will also enable the PI to accurately model the acceleration of solar energetic particles at CME shocks and other space weather phenomena. This research effort will involve student participation at all levels, including graduate students and postdocs, at the University of New Hampshire's Space Science Center.

PI和他的团队将构建一个基于物理的基于物理学的模型，以构建由谐振回旋体相互作用引起的所有冠状离子物种的动力学加速和加速度。他们将首先考虑质子的更现实的相互作用，考虑到波传播方向的广泛分布，这是观察结果所暗示的，并且通过其先前的可压缩MHD湍流中的工作所预测。该团队将将这种质子加热效应纳入流经冠状孔的血浆的空间演化中，然后他们将确定生成观察到的太阳风分布所需的详细波强度和光谱。由于α颗粒的光谱和波的分散关系将共同发展并相互影响，因此PI将使用混合模拟以自一看的方式对此行为进行建模。该模拟将遵循这些微物理分散相互作用，然后将其纳入全球冠状孔方程中，以描述径向位置增加的太阳风的巨摩托物演化。 PI的团队将使用这种努力而产生的动力学描述，以探索产生观察到的快速太阳风所需的谐振波光谱和光谱传输速率，以及流动性能对变化的冠状孔条件的响应。 PI还将将这种方法应用于无碰撞的慢性太阳风。对冠状血浆中发生的微物理过程的这种严格的动力学理解将使PI的团队能够在CME传播的全球模拟中正确重现干扰太阳风的热行为。这些知识还将使PI能够准确地对CME冲击和其他太空天气现象的太阳能颗粒的加速度进行建模。 这项研究工作将涉及新罕布什尔大学太空科学中心的各个级别的学生参与，包括研究生和博士后。