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

PI和他的团队将构建一个详细的基于物理的模型，描述由共振回旋相互作用引起的所有日冕空穴离子物种的动力学加热和加速。他们将首先研究更现实的质子相互作用，考虑到观测所暗示的波传播方向的广泛分布，以及他们先前在可压缩MHD湍流中所预测的。该团队将把这种质子加热效应纳入通过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。由于阿尔法粒子的光谱和波的色散关系将一起演化并相互影响，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弥散相互作用，然后将其并入全球日冕洞方程，以描述太阳风随径向位置增加的宏观物理演化。PI的团队将利用这项工作产生的动力学描述来探索产生所观测到的快速太阳风所需的共振波谱和光谱能量传输速率的极限，以及流动特性对日冕洞条件变化的响应。PI还将把这种方法应用于无碰撞的慢太阳风。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。这一知识还将使PI能够准确地模拟CME激波和其他空间天气现象中太阳高能粒子的加速。这项研究工作将吸引各级学生的参与，包括新汉普郡大学空间科学中心的研究生和博士后。

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.