SHINE: Using Two-Ribbon Flare Observations and Magnetohydrodynamics (MHD) Simulations to Study Eruptive Flares and Their Relationship to Coronal Mass Ejections (CMEs)

双带耀斑是最强大和潜在的地球效应类型的太阳耀斑。 这个为期3年的SHINE项目旨在研究太阳耀斑带的动力学，并将其与光球磁结构和日冕物质抛射（CME）的性质联系起来。 该团队将开发一个双带耀斑的集合数据库，并结合CME的磁流体动力学（MHD）模拟，以了解重连通量和CME特性之间的关系。 该项目解决了耀斑带如何发展的问题，以及它们如何与CME相关联，这对于理解太阳爆发的基本物理学非常重要。 基于大得多的数据集并由理论MHD背景支持的将大规模CME属性与源区耀斑属性相关联的能力将允许改进空间天气预报（例如，更准确的CME到达时间1 Au）和方法，解决了SHINE社区的主要目标和保护我们在太空中资产的能力。 该项目的科学成果将提高对太阳耀斑的科学和技术认识，使丹尼尔K. Inouye太阳望远镜（DKIST）和更现实和计算复杂的数据驱动的MHD模型的应用。 该研究项目将由加州大学伯克利分校的初级女科学家领导，她将与主办机构的几名本科生合作。 该项目的研究和EPO议程支持AGS部门在发现，学习，多样性，这个SHINE项目的目的是利用新组装的耀斑带图数据库，（在盘中心45度以内）和所有双带耀斑的重联通量（C1.0及以上）在太阳动力学天文台（SDO）时代观察到的，以研究带状物的属性是如何与其他耀斑和CME属性，无论是从观测和建模的角度来看。 对于所有事件，项目组将计算耀斑带内外的矢量磁场倾角、切变和垂直电流演化。 在CME观测允许的情况下，该团队将量化大规模CME属性之间的关系，包括CME速度，加速度和来自原位观测的行星际CME（ICME）的磁通量，并将其与上述带状物的属性进行比较。 对于与缓慢，中等和快速CME相关的三种不同的太阳爆发事件，研究人员将进行3D MHD模拟并分析其耀斑带和CME/ICME属性，以提供理论背景和指导，以充分理解观测结果。

Two-ribbon flares are the most powerful and potentially geoeffective type of solar flares. This 3-year SHINE project aims to investigate the dynamics of solar flare ribbons, and relate them to photospheric magnetic structures and properties of Coronal Mass Ejections (CMEs). The team will develop an ensemble database of the two-ribbon flares in combination with magnetohydrodynamic (MHD) simulations of CMEs to understand the relation between reconnection flux and CME properties. The project addresses the question of how flare ribbons develop, and how they are associated with CMEs, which is very important for understanding the fundamental physics of solar eruptions. The ability to relate large-scale CME properties to the source-region flare properties based on a much larger dataset and supported by theoretical MHD context will allow for improved space weather forecasts (e.g., more accurate CME arrival times at 1 AU) and methods, addressing the main goal of the SHINE community and the ability to protect our assets in Space. The scientific outcome of this project will enhance scientific and technological understanding of solar flares, enabling readiness for the Daniel K. Inouye Solar Telescope (DKIST) and application of more realistic and computationally sophisticated data-driven MHD models. The research project will be led by junior female scientist at UC Berkeley who will work with several undergraduate students at the host institution. The research and EPO agenda of this project supports the Strategic Goals of the AGS Division in discovery, learning, diversity, and interdisciplinary research.This SHINE project aims to utilize the newly assembled database of flare-ribbon maps (within 45 degrees of disk center) and reconnection fluxes of all two-ribbon flares (C1.0 and above) observed during the Solar Dynamics Observatory (SDO) era to investigate how ribbons properties are related to other flare and CME properties, both from the observational and modeling points of view. For all events, the project team will calculate vector magnetic field inclination, shear and the vertical electric current evolution inside and outside flare ribbons. Where CME observations permit, the team will quantify the relationship between large-scale CME properties, including the CME speed, acceleration and the magnetic flux from the in-situ observed interplanetary CME (ICME) and compare those with the ribbon's properties above. For three distinct events of solar eruptions associated with slow, moderate and fast CMEs, the investigators will perform 3D MHD simulations and analyze their flare ribbons and CME/ICME properties to provide the theoretical context and guidance to fully understand the observations.