Collaborative Research: SHINE: Laboratory, Observational, and Modeling Investigations of the Torus Instability and Associated Solar Corona Eruptive Phenomena

该研究项目将扩展对太阳日冕等离子体的理解，超越使用单一方法的可能性，例如只是分析数据，只是建模或只是做实验。 这些不同方法的交叉检查和讨论将提供一个强大的手段，进入问题的核心，并找出到底是怎么回事，通过协调第一原理模型，实验和观测分析，有一个很好的前景，实现长期寻求的见解和提高对太阳爆发机制的理解。 这一为期三年的合作项目将产生：㈠提高对日冕全球现象的认识，因为喷发通过释放磁能、磁螺旋度和等离子体粒子影响日冕的其余部分; ㈡提高对与喷发有关的现象的认识，如高能粒子和从无线电波到伽马射线的电磁辐射; ㈢增进对火山爆发对地球的影响的了解，例如对磁层和电离层、无线电传播和航天器的影响; ㈣由于实验、观测和数值模拟的高度直观性，提高了公众对太阳物理学的兴趣;以及㈤对学生进行太阳和等离子体物理学方面的培训，并支助一名年轻的女研究员。 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。这个为期3年的合作SHINE项目的主要目标是将实验室实验，实际太阳爆发数据分析和基本磁流体动力学（MHD）的数值模拟相结合。 具有与太阳等离子体类似的形态和动力学的实验室等离子体将由加州理工学院的研究人员进行研究。 这项研究是可行的，因为MHD没有内在的尺度，所以MHD实验室等离子体具有类似于日冕的无量纲数量和形态，将表现出类似的行为，但在不同的时间和空间尺度。 对实际太阳爆发和日冕物质抛射运动学的分析将在新泽西理工学院进行。 这一分析将集中在磁场结构特性和以上的喷发源区。 该分析将根据从航天器（如Hinode和SDO）获得的磁图数据进行非线性无力外推，以便计算作为高度和核心磁场函数的捆扎场分布。 CME的加速度曲线和最终速度对衰减指数的依赖关系将进行分析，并与实验和预测科学公司开发的数值模型进行比较。 项目小组将把数值预测与实验室实验和太阳喷发分析进行比较。 这种比较将考虑到两个捆扎场衰减指数和形态变化的爆发通量绳由于扭结。

This research project will extend understanding of solar corona plasmas beyond what is possible using single approaches, such as just analyzing data, just modeling, or just doing experiments. The cross-checking and discussion of these different approaches will provide a robust means for getting to the heart of the matter and finding out what is really going on. By reconciling first-principle models, experiments, and analysis of observations, there is an excellent prospect of achieving long-sought insights and improved understanding regarding underlying solar eruption mechanisms. This 3-year collaborative SHINE project would yield: (i) improved understanding of solar corona global phenomena since eruptions impact the remainder of the solar corona by shedding magnetic energy, magnetic helicity, and plasma particles; (ii) improved understanding of phenomena associated with eruptions such as energetic particles and electromagnetic radiation spanning from radio waves to gamma rays; (iii) improved understanding of the terrestrial impact of eruptions such as the effects on the magnetosphere and ionosphere, on radio propagation, and on spacecraft; (iv) increased public interest in solar physics, because of the highly visual nature of the experiments, the observations, and the numerical modeling; and, (v) training of students in solar and plasma physics and supporting a young female researcher. The research and EPO agenda of this project supports the Strategic Goals of the AGS Division in discovery, learning, diversity, and interdisciplinary research.The main goal of this 3-year collaborative SHINE project is to combine laboratory experiments, analysis of data from actual solar eruptions, and numerical modeling of the fundamental magnetohydrodynamics (MHD). Laboratory plasmas having morphology and dynamics similar to solar plasmas will be studied by at Caltech. This study is feasible because MHD has no intrinsic scale so MHD laboratory plasmas having dimensionless numbers and morphology similar to the solar corona will exhibit similar behavior, but on much different temporal and spatial scales. The analysis of actual solar eruptions and CME kinematics will be performed at the New Jersey Institute of Technology. This analysis will focus on the magnetic field structural properties in and above the source regions of eruptions. The analysis will apply non-linear force-free extrapolations based on magnetogram data obtained from spacecraft, such as Hinode and SDO, so as to calculate the strapping field profile as a function of altitude and core magnetic field. The dependence of CME acceleration profile and final speed on the decay index will be analyzed and compared to the experiments and to the numerical models developed at Predictive Science Inc. The project team will compare numerical predictions to both the laboratory experiments and the solar eruption analysis. This comparison will take into account both the strapping field decay index and morphological changes of erupting flux ropes due to kinking.