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力学(MHD)湍流之间的关系，包括太阳风中的可观测后果，如内风的特征各向异性和外部日光层各种涨落的标度。描述本地MHD湍流长波和低频变化的输运理论将进一步被用来解决太阳风中的重要观测问题。这一理论的扩展将描述与上游波有关的波-粒子相互作用注入的波的同化，以及与新生的彗星和星际离子的拾取和同化有关的波。MHD基础理论的进一步工作将包括发展和完善基于信息熵描述的MHD驰豫过程的现象学，该描述最近在二维流体动力学湍流的背景下显示出希望。最后，研究人员将在太阳风加速的自洽模型中建立包括湍流效应的模型，并为彗星和激波附近的带电粒子波湍流动力学建立自洽模型。

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.