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详细的基于物理的模型，用于研究共振回旋加速器相互作用引起的所有冕洞离子物种的动力学加热和加速。他们将首先研究质子的更现实的相互作用，考虑到波传播方向的广泛分布，正如观测所暗示的那样，也正如他们先前在可压缩MHD湍流中的工作所预测的那样。该团队将把这种质子加热效应纳入通过日冕洞向外流动的等离子体的空间演化中，然后他们将确定产生观测到的太阳风分布所需的详细波强度和光谱。由于α粒子的光谱和波的色散关系将一起演变并相互影响，PI将使用混合模拟以自洽的方式对这种行为进行建模。模拟将遵循这些微物理色散相互作用，然后将其纳入全球冕洞方程，以描述太阳风随径向位置增加的宏观物理演变。PI的团队将使用这项工作产生的动力学描述来探索产生观测到的快速太阳风所需的共振波谱和光谱能量传输率的限制，以及流动特性对不断变化的冕洞条件的响应。PI还将把这种方法应用于无碰撞的慢速太阳风。对日冕等离子体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地再现扰动太阳风的热行为。这些知识还将使PI能够准确地模拟太阳高能粒子在CME冲击和其他空间天气现象中的加速。 这项研究工作将涉及各级学生的参与，包括研究生和博士后，在新罕布什尔州的空间科学中心的大学。