NSWP: Tomographic Reconstruction of the 3-D Coronal Magnetic Field from Space- and Ground-Based Intensity and Polarimetry Data

NSWP：根据天基和地基强度和偏振数据对 3-D 日冕磁场进行层析成像重建

• 批准号: 0819971
• 负责人: Hao Sheng Lin
• 金额: $ 55.99万
• 依托单位: University of Hawaii
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2008
• 资助国家: 美国
• 起止时间: 2008-11-01 至 2014-10-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0819971&HistoricalAwards=false
• 关键词: NSWP; Tomographic; Reconstruction; Coronal; Magnetic

The Principal Investigator (PI) will integrate current space-based and ground-based observing capabilities with new data analysis techniques, in order to develop scalar and vector tomography tools for reconstructing the Sun's 3D coronal magnetic field configuration. The PI will utilize ground-based measurements of coronal magnetic fields through near-IR spectropolarimetric observations, stereoscopic coronal imaging from NASA's STEREO (Solar TErrestrial RElations Observatory) mission, and coronal vector tomography techniques to develop these new space weather tools. He will then use the resulting 3D coronal reconstructions to test theoretical coronal magnetic field models, as well as to study coronal magnetic field configuration variations of active regions, before and after the occurrence of flares and coronal mass ejections (CMEs). The PI's goal to directly infer the 3D structure of coronal magnetic fields from observations is of fundamental importance to solar physics. This project will increase our understanding of the physical mechanisms responsible for the heating of the solar corona, the generation of solar EUV radiation, and the origin of fast and slow solar winds. The proposed research will lead to a better understanding of the energetic solar events that drive space weather, and thus enhance our predictive capabilities for such events.

首席研究员将把目前的天基和地基观测能力与新的数据分析技术结合起来，以便开发标量和矢量层析成像工具，用于重建太阳的三维日冕磁场结构。PI将通过近红外分光偏振观测、美国宇航局STEREO（日地关系观测站）使命的立体日冕成像和日冕矢量层析成像技术，利用地面日冕磁场测量来开发这些新的空间天气工具。然后，他将使用由此产生的3D日冕重建来测试理论日冕磁场模型，并研究耀斑和日冕物质抛射（CME）发生前后活动区域的日冕磁场配置变化。PI的目标是从观测中直接推断日冕磁场的3D结构，这对太阳物理学至关重要。该项目将增加我们对太阳日冕加热、太阳极紫外辐射产生以及快速和慢速太阳风起源的物理机制的理解。拟议的研究将有助于更好地了解驱动空间天气的高能太阳事件，从而提高我们对此类事件的预测能力。