GEM: Solar Wind Entry into the Magnetospohere and Its Paths to the Plasma Sheet

GEM：太阳风进入磁球及其到达等离子体片的路径

• 批准号: 0502992
• 负责人: Nojan Omidi
• 金额: $ 74.99万
• 依托单位: Solana Scientific Inc.
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2005
• 资助国家: 美国
• 起止时间: 2005-09-15 至 2010-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0502992&HistoricalAwards=false
• 关键词: GEM; Solar; Wind; Entry; into

How and where plasma from the solar wind enters Earth's magnetosphere is still largely unknown. This project will use a combination of state-of-the-art global hybrid (kinetic ions, fluid electrons) simulations and comparison with spacecraft data to address this problem. The project has two phases. The first concerns the entry of plasma into the magnetosphere on the dayside magnetopause, while the second concerns phenomena that occur on the magnetotail flanks and the processes that transfer incoming solar wind plasma into the plasma sheet. Initially, the focus will be on issues such as the influences of the bow shock, ion foreshock and magnetosheath on dayside transport during steady and non-steady solar wind conditions. Formation of low latitude (LLBL) and high latitude (HLBL) boundary layers and their structure will be investigated. Next, the transport of the boundary layer plasma will be followed to assess its contributions to the plasma sheet population. In addition, direct entry mechanisms into the plasma sheet through the tail lobes and flanks will be investigated. The proposed modeling and spacecraft data analysis activities are designed to take advantage of the strength of each approach and achieving a synergy that will lead to an understanding of solar wind entry into the magnetosphere and its paths to the plasma sheet. By virtue of resolving ion temporal and spatial scales, global hybrid simulations are uniquely suited for addressing plasma transport questions such as the relative significance of reconnection and wave-particle interactions or local vs. non-local processes. In addition to the basic plasma moments (density, flow speed etc.), hybrid simulations will provide ion velocity distribution functions throughout the magnetosphere. The kinetic treatment of ions makes it possible to investigate mass filtering effects at the magnetopause and to trace the orbit of ions in a self consistent manner.

来自太阳风的等离子体如何以及在哪里进入地球磁层在很大程度上仍然是未知的。该项目将结合最先进的全球混合(动能离子、流体电子)模拟和与航天器数据的比较来解决这一问题。该项目分为两个阶段。第一个涉及日侧磁层顶上的等离子体进入磁层，第二个涉及发生在磁尾侧翼的现象以及将传入的太阳风等离子体转移到等离子体片中的过程。最初，重点将放在稳定和非稳定太阳风条件下弓激波、离子前震和磁鞘对白天交通的影响等问题上。将研究低纬和高纬边界层的形成及其结构。下一步，将跟踪边界层等离子体的传输，以评估其对等离子体片总体的贡献。此外，还将研究通过尾叶和侧翼直接进入等离子体片的机制。拟议的建模和航天器数据分析活动旨在利用每种方法的优势，实现协同作用，从而有助于了解太阳风进入磁层及其到达等离子体片的路径。由于能够分辨离子的时间和空间尺度，全球混合模拟特别适合于解决等离子体输运问题，例如重联和波粒相互作用的相对重要性，或者局部过程与非局部过程的相对重要性。除了基本的等离子体矩(密度、流速等)外，混合模拟还将提供整个磁层的离子速度分布函数。离子的动力学处理使研究磁层顶的质量过滤效应和以自洽的方式追踪离子的轨道成为可能。