SHINE: A Time-Dependent Solar Wind 3D-MHD Model Interface Using Interplanetary Scintillation (IPS) Observations

这个为期3年的SHINE项目的主要目标是将层析分析应用于现有的行星际闪烁（IPS）遥感观测和SMEI（太阳质量抛射成像仪）档案白光观测的日球层数据，并将该技术扩展到STEREO航天器上的HI-2（日球层成像仪-2）仪器。这项研究工作将使项目团队能够发现他们自己对这些参数在地球附近的运动传播的可靠测量与使用三维（3D）磁流体动力学（MHD）模型控制太阳表面附近特征传播的物理过程之间的差异。该项目有助于更广泛的社会活动，例如促进妇女参与科学和提高公众的科学素养。项目团队将在国家科学会议上介绍该研究项目的结果，并将在同行评审的科学期刊上发表。SHINE项目的研究和EPO议程支持AGS部门在发现、学习、多样性和跨学科研究方面的战略目标。SHINE项目的研究议程包括四个主要任务，即：(i)比较加州大学圣地亚哥分校（UCSD）层析成像与MHD建模，以了解这两种截然不同类型的遥感分析之间的物理差异；（ii）对所有使用相同边界条件的3D MHD建模技术进行相互比较，以学习传播时间相关结构所需的最佳物理参数；（iii）对这些行星际结构进行分析，以确定并提供层析运动学模型传播所需的缺乏磁场输入；（iv）使用迭代的3D MHD代码进行新的分析，这些代码改进了来自太阳日球层观测和IPS测量的遥感观测。该研究项目的结果预计将产生新的改进边界输入，基于多个数据集（包括遥感观测和现场测量），用于各种3D MHD模型，特别是空间天气模型，以及显示日球层结构全球特性的分析。该项目将为“日冕物质抛射的太阳周期依赖性，包括它们通过背景太阳风的传播和相互作用，包括行星际和近太阳现象的联系”提供新的物理见解，正如美国国家科学基金会SHINE计划的目标所述。

The main goal of this 3-year SHINE project is to apply the tomographic analysis to heliospheric data from available remote-sensing observations of interplanetary scintillation (IPS), archival white-light observations from SMEI (Solar Mass Ejection Imager), and extend this technique to the HI-2 (Heliospheric Imager-2) instruments onboard the STEREO spacecraft. This research effort will allow the project team to discover the differences between their own robust measurements of the kinematic propagation of these parameters near the Earth and the physical processes governing the propagation of features from near the solar surface using three-dimensional (3D) magnetohydrodynamic (MHD) models. The project contributes to broader societal activities, such as advancing the participation of women in science and improving the scientific literacy of the general public. The project team will present the results of this research project at national scientific meetings and will publish them in peer-reviewed scientific journals. The research and EPO agenda of this SHINE project supports the Strategic Goals of the AGS Division in discovery, learning, diversity, and interdisciplinary research.The research agenda of this SHINE project consists of four main tasks, namely: (i) compare the University of California in San Diego (UCSD) tomographic modeling with MHD modeling to learn the physical differences between these two very different types of remote sensing analyses; (ii) pursue inter-comparison of 3D MHD modeling techniques that all use the same boundary conditions in order to learn the best physical parameters needed to propagate time-dependent structures; (iii) perform analysis of these interplanetary structures in order to determine and provide the lacking magnetic field inputs required for the tomographic kinematic model propagation; and, (iv) perform new analyses using iterative 3D MHD codes that refine remote sensing observations from solar heliospheric observations and IPS measurements. The outcome of this research project is expected to yield new improved boundary inputs, based on multiple data sets (that incorporate both remote-sensing observations and in-situ measurements), for various 3D MHD models, and especially for Space Weather models, and an analysis that displays the global properties of heliospheric structures. The project would provide new physical insight on "the solar cycle dependence of CMEs, including their propagation through and their interaction with the background solar wind, including the linking of interplanetary and near-Sun phenomena," as stated in the goals of the NSF's SHINE program.