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湍流之间的关系，包括太阳风中可观察到的后果，如内风的特征各向异性和日光层外层各种波动的比例。 将进一步利用描述局部MHD湍流的长波长和低频变化的传输理论来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。 在基本MHD理论的进一步工作将包括发展和完善的MHD弛豫过程的基础上的信息熵的描述，最近显示出的承诺，在二维流体力学湍流的情况下的现象。 最后，研究人员将建立模型，包括太阳风加速自洽模型中的湍流效应，以及彗星和冲击附近带电粒子波湍流动力学的自洽模型。

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.