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

这项研究项目将扩展对太阳电晕等离子体的理解，超越使用单一方法的可能性，例如仅仅分析数据，仅仅建模，或者仅仅做实验。对这些不同方法的相互核对和讨论将为深入问题的核心和查明真正发生的事情提供强有力的手段。通过协调第一性原理模型、实验和对观测的分析，很有可能实现长期寻求的见解和对潜在太阳喷发机制的更好理解。这一为期3年的合作项目将产生以下成果：(I)提高对太阳日冕全球现象的理解，因为喷发通过释放磁能、磁螺旋度和等离子体粒子影响太阳日冕的其余部分；(Ii)提高对与喷发相关的现象的理解，例如高能粒子和从无线电波到伽马射线的电磁辐射；(Iii)提高对喷发对地球的影响的理解，例如对磁层和电离层、对无线电传播和对航天器的影响；(Iv)提高公众对太阳物理学的兴趣，因为实验、观测和数值模拟的高度可视化；以及，(V)对学生进行太阳能和等离子体物理方面的培训，并支持一名年轻的女研究人员。这个项目的研究和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SISH项目的主要目标是结合实验室实验、实际太阳喷发数据的分析和基本磁流体动力学(MHD)的数值模拟。具有类似太阳等离子体的形态和动力学的实验室等离子体将由美国加州理工大学进行研究。这项研究是可行的，因为MHD没有本征尺度，所以具有与日冕相似的无量纲数和形态的MHD实验室等离子体将表现出相似的行为，但在时间和空间尺度上有很大不同。对实际太阳喷发和CME运动学的分析将在新泽西理工学院进行。这一分析将侧重于喷发源区域及其上方的磁场结构特性。分析将根据从Hinode和SDO等航天器获得的磁图数据进行非线性无力外推，以计算作为高度和核心磁场函数的束带场分布。将分析CME加速剖面和最终速度对衰变指数的依赖关系，并与实验和预测科学公司开发的数值模型进行比较。该项目团队将把数值预测与实验室实验和太阳喷发分析进行比较。这一比较既考虑了束带场衰减指数，又考虑了由于扭结而产生的喷发磁力绳的形态变化。

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.