Numerical Modeling of Reconnection-Generated Transients in the Solar Corona

太阳风的起源和演化、爆发太阳耀斑及其产生的日冕物质抛射(日冕物质抛射)是太阳-日球层联系的基本组成部分，对空间气象预报至关重要。这项工作将在促进教学、培训和学习的同时促进发现，并将通过网络和伙伴关系加强研究和教育的基础设施。该项目将支持一名博士后研究员，并为本科生的暑期研究项目提供便利。该项目的成果将广泛传播，因为PI、博士后学者和本科生将在国家和国际科学会议(如NSF SHELE研讨会)、座谈会和研讨会以及同行评议的期刊上展示他们的成果。近十年来在1AU对行星际磁通量绳进行现场观测的一个重要结果是，慢太阳风中大尺度CME磁绳和无处不在的小尺度磁绳的尺寸分布明显呈现出两个截然不同的群体，而遥感观测表明，它们的形成过程中日冕条件发生了巨大的变化。这项工作是对太阳喷发结构的多尺度性质进行的全面、多学科的调查。科学的主要目标是确定：(1)太阳和日球层磁通量绳的性质如何在它们的空间和能量尺度范围内变化，以及冕源区的局部和全球拓扑如何影响爆发瞬变及其所产生的磁结构的重联形成机制(S)；从根本上比较了来自伪流光的流光斑点、耀斑重联等离子体、流星绳和准流光绳喷发与来自流光喷发和强场活动区的经典大尺度日冕物质抛射的异同；每一群磁绳瞬变如何与其覆盖/相邻的磁通系统、开闭场边界和周围的太阳风流出相互作用。每个科学目标都将结合最先进的、高性能的数值模拟以及对多航天器遥感和现场观测的详细分析来解决。这一奖项反映了NSF的法定使命，并通过使用基金会的智力优势和更广泛的影响审查标准进行评估，被认为值得支持。

The origin and evolution of the solar wind and the initiation of eruptive solar flares and their resulting coronal mass ejections (CMEs) are fundamental building blocks of the solar–heliospheric connection and crucial for space weather forecasting. This work will advance discovery while promoting teaching, training, and learning and will enhance the infrastructure for research and education through networks and partnerships. The project will support a postdoctoral fellow and facilitate summer research projects for undergraduate students. Results from the project will be disseminated broadly as the PI, postdoctoral scholar, and undergraduate students will present their results at national and international scientific meetings (e.g. the NSF SHINE Workshop), in colloquia and seminars, and in peer-reviewed journals. One of the key results from the last decade of in-situ observations of interplanetary magnetic flux ropes at 1 AU is that the size distribution of large-scale CME flux ropes and the ubiquitous small-scale flux ropes in the slow solar wind apparently show two distinct populations while remote sensing observations indicate tremendous variation of coronal conditions during their formation. This work is a comprehensive, multidisciplinary investigation into the multi-scale nature of solar eruptive structures. The main Science Objectives are to determine: (1.) How solar and heliospheric magnetic flux rope properties vary over their range of their spatial and energy scales and how the local and global topologies of coronal source regions influence the reconnection formation mechanism(s) of eruptive transients and their resulting magnetic structure; (2.) The fundamental similarities and differences between streamer blob flux ropes, flare reconnection plasmoids, flux rope and quasi-flux rope eruptions from pseudostreamers, and classic, large-scale CMEs from streamer blowouts and stronger-field active regions; (3.) How each of these populations of flux rope transients interact with their overlying/adjacent flux systems, the open-closed field boundaries, and the ambient solar wind outflow. Each of the Science Objectives will be addressed with a combination of state-of-the-art, high-performance numerical modeling along with detailed analysis of multi-spacecraft remote sensing and in-situ observations.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.