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

双带状耀斑是太阳耀斑中最强大、最具地球效应的一种。这个为期3年的SHINE项目旨在研究太阳耀斑带的动力学，并将它们与日冕物质抛射（cme）的光球磁结构和性质联系起来。该团队将结合日冕物质抛射的磁流体动力学（MHD）模拟，开发一个双带状耀斑的集合数据库，以了解重联通量和日冕物质抛射特性之间的关系。该项目解决了耀斑带是如何发展的问题，以及它们与日冕物质抛射的关系，这对于理解太阳爆发的基本物理学非常重要。基于更大的数据集，并在理论MHD背景的支持下，将大规模CME属性与源区域耀斑属性联系起来的能力将允许改进空间天气预报（例如，更准确的CME到达1 AU的时间）和方法，解决SHINE社区的主要目标和保护我们在空间中的资产的能力。该项目的科学成果将增强对太阳耀斑的科学和技术理解，为Daniel K. Inouye太阳望远镜（DKIST）做好准备，并应用更现实、计算更复杂的数据驱动MHD模型。该研究项目将由加州大学伯克利分校的年轻女性科学家领导，她将与该校的几名本科生合作。该项目的研究和EPO议程支持AGS部门在发现、学习、多样性和跨学科研究方面的战略目标。SHINE项目旨在利用太阳动力学观测站（SDO）时代观测到的所有双带耀斑（C1.0及以上）的新建立的耀斑-带状地图数据库（距离圆盘中心45度以内）和重联通量，从观测和建模的角度研究带状特性与其他耀斑和CME特性之间的关系。对于所有事件，项目组将计算矢量磁场倾角、剪切和耀斑带内外的垂直电流演变。在CME观测允许的情况下，研究小组将量化大规模CME特性之间的关系，包括CME的速度、加速度和来自原位观测的行星际CME （ICME）的磁通量，并将这些与上面的带状特性进行比较。对于与慢、中、快CME相关的三种不同的太阳喷发事件，研究人员将进行3D MHD模拟，并分析它们的耀斑带和CME/ICME特性，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.