SHINE: Constraining Solar Wind and Coronal Mass Ejection (CME) Models Using in situ Ionic Composition Observations

SHINE：使用原位离子成分观测约束太阳风和日冕物质抛射 (CME) 模型

• 批准号: 0454596
• 负责人: Thomas Zurbuchen
• 金额: $ 29.98万
• 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: 2005
• 资助国家: 美国
• 起止时间: 2005-01-01 至 2008-12-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0454596&HistoricalAwards=false
• 关键词: SHINE; Constraining; Solar; Wind; Coronal

The PI proposes to utilize and model in situ solar wind charge states measured by the Advanced Composition Explorer (ACE) and Ulysses spacecraft since 1998. He plans to solve critical science questions regarding the source and acceleration of the slow and fast solar wind, the boundaries separating them, and the initiation mechanism of Interplanetary Coronal Mass Ejections (ICMEs). The proposed work will require collaboration between solar and heliospheric physicists and lead the SHINE community to an improved understanding of the corona and heliospheric systems as a whole. This dedicated effort seeks to reconcile theories with observations, enabling the determination of compositional and thermal constraints for CME and solar wind models. Solar wind ionic composition is a unique and important measure of the thermal environment of its coronal source region, as well as the source regions of plasma associated with ICMEs. Charge states in the solar wind reflect the electron temperatures in the inner corona, and the thermal history of the solar wind can be used to determine expansion properties and heat deposition in the low corona. This effort builds upon previous work that has shown that ionic charge states of heliospheric plasmas are crucial in identifying ICMEs and analyzing the sources of energetic particles accelerated in the heliosphere. The proposers will develop a freeze-in code to model the expansion and ionization of solar wind ions under a variety of coronal conditions. They will apply physics models that will enable the calculation and comparison of the modeled coronal electron temperatures with the observed ionization states from in situ data. The PI will subsequently construct radial temperature profiles by considering ions that freeze-in at different heliocentric radii. The results of the proposed work will provide the most comprehensive analysis of the thermal history of the solar wind close to the Sun, based on a complete set of measurements of in situ ionization states.

PI提议以自1998年以来由高级组成资源管理器（ACE）和Ulysses航天器测量的原位太阳能电荷状态使用和建模。将它们分开，以及星际冠状质量弹出（ICMES）的起始机理。拟议的工作将需要太阳能和地球物理学家之间的合作，并使Shine社区对整个电晕和地球层系统有了深入的了解。这项敬业的努力旨在使理论与观察结果调和，从而确定CME和太阳风模型的组成和热约束。太阳风离子组成是其冠状动脉源区域热环境以及与ICME相关的血浆源区域的独特而重要的度量。太阳风中的电荷状态反映了内部电晕中的电子温度，可用于确定低电晕中的太阳风的热历史和热量沉积。这项工作基于以前的工作，这表明地球层等离子体的离子电荷状态对于识别ICME和分析在地球层加速的能量颗粒来源至关重要。提议者将开发一个冷冻代码，以在多种冠状条件下建模太阳能离子的扩展和电离。他们将采用物理模型，以实现建模的冠状电子温度与观察到的电离状态的原位数据的计算和比较。 PI随后将通过考虑在不同的中心半径上冻结的离子来构建径向温度曲线。拟议工作的结果将根据原位离子化状态的一组测量值，对靠近太阳的太阳风的热历史进行最全面的分析。