Magnetohydrodynamic Turbulence and Turbulence in the Interplanetary Medium

该项目将研究不可压缩和可压缩磁流体动力学（MHD）湍流之间的关系，包括太阳风的可观测结果，如内风的特征各向异性和外日球层各种波动的标度。描述局地MHD湍流的长波长和低频变化的输运理论将被进一步开发，以解决太阳风中的重要观测问题。该理论的扩展将描述与上游波相关的波粒相互作用注入的波的同化，以及与新生彗星和星际离子的拾取和同化相关的波。基础MHD理论的进一步工作将包括基于信息熵描述的MHD弛豫过程现象学的发展和完善，该描述最近在二维流体动力学湍流背景下显示出前景。最后，研究人员将构建包括湍流效应在内的太阳风加速自一致模型，以及彗星和冲击附近带电粒子波湍流动力学自一致模型。

This project will research the relationship between incompressible and compressible magnetohydrodynamic (MHD) turbulence, including observable consequences in the solar wind, such as characteristic anisotropies in the inner wind and scalings of various fluctuations in the outer heliosphere. A transport theory for description of the long wavelength and low frequency variations of local MHD turbulence will be further exploited to address important observational issues in the solar wind. Extensions of this theory will describe assimilation of waves injected by wave-particle interactions associated with upstream waves, as well as waves associated with pickup and assimilation of newborn cometary and interstellar ions. Further work in basic MHD theory will include development and refinement of a phenomenology of MHD relaxation processes based upon an information-entropy description which has recently shown promise in the context of two dimensional hydrodynamics turbulence. Finally, the investigators will construct models for including turbulence effects in self- consistent models of solar wind acceleration, and self-consistent models for charged particle-wave turbulence dynamics near comets and shocks.