Comparative Studies of the Interaction and Ionospheric Processes at a Variety of Different "Non-Magnetic" Solar System Bodies

各种不同“非磁性”太阳系天体相互作用和电离层过程的比较研究

• 批准号: 0845133
• 负责人: Andrew Nagy
• 金额: $ 30.34万
• 依托单位: Regents of the University of Michigan - Ann Arbor
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2009
• 资助国家: 美国
• 起止时间: 2009-02-01 至 2013-01-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0845133&HistoricalAwards=false
• 关键词: Comparative; Studies; Interaction; Ionospheric; Processes

This project provides continuing support to enable extension of previously funded investigation of the interaction of fast flowing plasma with non-magnetized solar system bodies. In the previous project, comprehensive numerical schemes that had been developed for terrestrial space weather applications were modified to be used for a variety of solar system applications. A significant fraction of the effort centered on the development, in a systematic fashion, of the "best possible" magnetohydrodynamic (MHD) models to describe these interactions and ionospheric phenomena at Titan and Mars. The result is a high spatial resolution, multi-species, spherical, Hall, magnetohydrodynamic model that can calculate the solar wind interaction processes, escape fluxes, and associated ionospheric phenomena. The spherical model has a grid resolution of about 10 km and 35 km in the ionospheric regions of Mars and Titan, respectively, providing very good simulations of the measured densities. This project will expand the effort to include other solar system bodies in order to undertake comparative studies; of particular interest are Io, Europa, Callisto, and Enceladus. The MHD code will be modified to be multi-fluid by solving separate momentum and energy equations for the different species. The codes will be applied to investigations of the many similarities and the important differences in the chemical and physical processes associated with the different solar system bodies. The numerical schemes to be used originated in the field of computational fluid dynamics and will likely find applications outside the field of planetary and comparative aeronomy, such as global climate change modeling. The basic MHD code that is being continually improved will be useful in current space weather efforts. The project will provide partial support for a female graduate student.

该项目提供持续的支助，以扩大以前资助的对快速流动等离子体与非磁化太阳系天体相互作用的研究。在上一个项目中，对为地面空间气象应用开发的综合数值方案进行了修改，以便用于各种太阳系应用。很大一部分的努力集中在发展，在一个系统的方式，“最好的”磁流体动力学（MHD）模型来描述这些相互作用和电离层现象在土卫六和火星。其结果是一个高空间分辨率，多物种，球形，霍尔，磁流体动力学模型，可以计算太阳风的相互作用过程，逃逸通量，和相关的电离层现象。 球形模型在火星和土卫六的电离层区域的网格分辨率分别为10公里和35公里，可以很好地模拟测量的密度。这一项目将扩大努力范围，将太阳系其他天体包括在内，以便进行比较研究;特别感兴趣的是木卫一、木卫二、木卫四和土卫二。 通过求解不同物质的动量和能量方程，将MHD代码修改为多流体。这些代码将用于研究与太阳系不同天体有关的化学和物理过程中的许多相似之处和重要差异。拟使用的数值方案源自计算流体动力学领域，可能会在行星和比较高空大气学领域之外找到应用，如全球气候变化建模。正在不断改进的基本MHD代码将在当前的空间气象工作中发挥作用。 该项目将为一名女研究生提供部分支助。