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

国际和平研究所建议利用自1998年以来由先进成分探测器(ACE)和尤利西斯航天器测量的太阳风电荷态并对其进行模拟。他计划解决有关慢速和快速太阳风的来源和加速、分隔它们的边界以及行星际日冕物质抛射(ICME)的启动机制等关键科学问题。这项拟议的工作将需要太阳和日球层物理学家之间的合作，并引导SIRE社区更好地了解日冕和日球层系统作为一个整体。这项专心致志的工作试图调和理论与观测，从而能够确定CME和太阳风模型的成分和热约束。太阳风离子组成是衡量日冕源区以及与ICME有关的等离子体源区热环境的一项独特而重要的指标。太阳风中的电荷态反映了内日冕中的电子温度，太阳风的热历史可以用来确定低日冕中的膨胀性质和热沉积。这项工作是在以前工作的基础上进行的，这些工作表明，日光层等离子体的离子电荷态对于确定冰盖机械系统和分析在日光层加速的高能粒子的来源至关重要。提出者将开发一个冻结代码，以模拟各种日冕条件下太阳风离子的膨胀和电离。他们将应用物理模型，能够计算模拟的日冕电子温度，并将其与从现场数据观测到的电离态进行比较。PI随后将通过考虑冻结在不同日心半径的离子来构建径向温度分布。这项拟议工作的结果将基于一套完整的原位电离态测量结果，对靠近太阳的太阳风的热历史提供最全面的分析。

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.