SHINE: Driving Global Heliospheric Magnetohydrodynamics (MHD) Models with Tomographically-Determined Lower Boundary Conditions

SHINE：利用断层扫描确定的下边界条件驱动全球日光层磁流体动力学 (MHD) 模型

• 批准号: 0555561
• 负责人: Farzad Kamalabadi
• 金额: $ 38.95万
• 依托单位: University of Illinois at Urbana-Champaign
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2006
• 资助国家: 美国
• 起止时间: 2006-01-01 至 2008-12-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0555561&HistoricalAwards=false
• 关键词: SHINE; Driving; Global; Heliospheric; Magnetohydrodynamics

The aim of this proposal is to drive existing three-dimensional (3D) heliospheric magnetohydrodynamics (MHD) models with tomographically determined values of electron density (Ne) and temperature (T) at the lower solar boundary. These new heliospheric models then will be used to study the quasi-steady solar wind, coronal mass ejection (CME) propagation, CME-driven shocks, and the associated energetic particle events. The sources of data for the tomographic determinations will be the Mark IV white-light coronagraph at Mauna Loa Solar Observatory, the COR1 (white-light coronagraph for inner corona) coronagraph on STEREO (solar terrestrial relations observatory), SXT (soft X-ray telescope) on Yohkoh, EUVI (extreme ultraviolet imager) on STEREO, EIT (extreme ultraviolet imaging telescope) on SOHO (solar and heliospheric observatory), XRT (X-ray telescope) on Solar-B, and AIA (atmospheric imaging assembly) on the Solar Dynamics Observer spacecraft. In this three-year collaborative project, the University of Illinois will generate the 3D tomographic models and use them to specify lower boundary conditions for the University of Michigan 3D heliosphere model based on the BATS-R-US MHD code. The current generation of 3D heliospheric models uses synoptic magnetograms to establish the magnetic field at the lower boundary. Determination of the lower boundary values of Ne and T is far more problematic, and researchers are compelled to use simplistic assumptions (such as that the density can be related to the magnetic field magnitude by a scale factor). Tomography offers an excellent opportunity to determine realistic boundary values of Ne and T in the corona. The tomographic models developed under this research grant will have numerous applications, including determining the constraints on coronal heating functions and providing a 3D context to help interpret high-resolution ultra-violet (UV) spectra. This project will support an interdisciplinary collaboration between the Department of Electrical and Computer Engineering at the University of Illinois and Department of Ocean, Atmospheric and Space Science at the University of Michigan, and will directly support undergraduate and graduate education.

该建议的目的是驱动现有的三维（3D）日光层磁流体动力学（MHD）模型与层析X射线摄影确定的电子密度（Ne）和温度（T）的值在较低的太阳边界。这些新的日光层模型将被用来研究准稳态太阳风、日冕物质抛射（CME）传播、CME驱动的激波以及相关的高能粒子事件。断层摄影测定的数据来源将是莫纳罗亚太阳天文台的Mark IV白光日冕仪，COR 1（白光电晕灯用于内电晕）立体声电晕灯（日地关系观测台）（软X射线望远镜）位于EUVI Yohkoh（极紫外成像仪）在STEREO，EIT SOHO（太阳和日光层观测台）上的极紫外成像望远镜、Solar-B上的XRT（X射线望远镜）和太阳动力学观测器航天器上的AIA（大气成像组件）。在这个为期三年的合作项目中，伊利诺伊大学将生成3D断层模型，并使用它们来指定基于BATS-R-US MHD代码的密歇根大学3D日光层模型的下边界条件。目前的三维日光层模型使用天气磁图来建立下边界的磁场。确定Ne和T的下边界值要困难得多，研究人员不得不使用简单的假设（例如密度可以通过比例因子与磁场大小相关）。断层扫描提供了一个很好的机会，以确定现实的边界值Ne和T的电晕。在这项研究资助下开发的层析成像模型将有许多应用，包括确定日冕加热功能的约束条件，并提供3D背景，以帮助解释高分辨率的紫外线（UV）光谱。该项目将支持伊利诺伊大学电气和计算机工程系与密歇根大学海洋、大气和空间科学系之间的跨学科合作，并将直接支持本科和研究生教育。