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

PI计划利用并模拟自1998年以来由高级成分探测器（ACE）和尤利西斯航天器测量的太阳风电荷状态。他计划解决有关慢速和快速太阳风的来源和加速度、它们之间的边界以及行星际日冕物质抛射（ICMEs）的启动机制等关键科学问题。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SHINE社区提高对日冕和日球层系统的整体理解。这项专门的工作旨在使理论与观测相协调，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其日冕源区热环境的一个独特而重要的指标，也是与ICMEs相关的等离子体源区。太阳风中的电荷状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特性和热沉积。这项工作建立在先前的工作基础上，该工作表明，日球等离子体的离子电荷状态对于识别ICMEs和分析日球层中加速的高能粒子的来源至关重要。提议者将开发一个冻结代码来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，使模拟的日冕电子温度与从原位数据中观察到的电离状态进行计算和比较。PI随后将通过考虑在不同日心半径处冻结的离子来构建径向温度分布。这项工作的结果将基于一套完整的原位电离状态测量，对太阳风靠近太阳的热历史进行最全面的分析。

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.