Revealing Evolution of Electrons and Magnetic Field in Solar Flares

现代太阳物理学通过新的观测探索太阳，其光谱覆盖范围以及空间，光谱和时间分辨率相对于几年前有了惊人的改善，这是由于最近的技术进步。 与此同时，数据的复杂性和数量也成比例地增加。 这个为期三年的项目的主要目标是将这些多维观测与理论，分析工具和建模紧密结合，以获得新的知识并在太阳物理学方面做出基础科学发现，特别是关于太阳活动的物理驱动因素的性质。 太阳活动主要取决于日冕的磁性，广义上说，包括磁场的产生、形态/拓扑的控制、时间演化、日冕中动能、热能和非热能的转化，以及磁结构和热结构之间的耦合。 测量日冕磁场及其在动态时间尺度上的变化的能力是揭示驱动太阳耀斑，爆发和活动的基本物理学的关键。 虽然一直缺乏可靠的直接测量日冕磁场，但该项目旨在充分利用最终可用的大量高分辨率数据和建模，从根本上改变这种情况。 具体地说，新的、功能齐全的微波干涉仪-NJIT的扩大欧文斯谷太阳能阵列（EOVSA）-最近首次提供了一个实际机会，可以经常利用日冕的无线电观测来探测太阳耀斑所涉及的磁结构，该干涉仪已开始对太阳进行定期的干涉观测。 为了理解这些数量和复杂性逐渐增加的高要求数据，并将这些数据与太阳耀斑中加速的非热电子沿着纳入磁和热结构的完整合成图，该项目将利用复杂的模型，这些模型将联合收割机结合最先进的理论，计算代码，该项目包括广泛传播在太阳射电天文学方面收集到的新知识，以增进不仅在太阳物理学方面，而且在整个天体物理学方面的科学认识。 EOVSA观测的基本性质确保了对太阳物理学领域的广泛影响，包括DIKIST，FASR等未来仪器的开发工作将导致用户友好的软件工具，将通过Solarsoft IDL分发库广泛提供给太阳和空间气象社区。 这些建模工具将在NJIT的太阳-地球研究中心（CSTR）的夏季实习期间使用，项目团队招募当地初中生参与尖端太阳能研究。 此外，在NJIT的CSTR提供的高度多样化的环境中进行，各种项目活动将促进发现和理解，同时促进教学，培训和学习。 特别是，易于使用的工具将在这个项目期间开发，使伟大的学习工具，将广泛用于研究生课程在CSTR，如“射电天文学”，“太阳物理学”和“等离子体物理学和磁流体动力学。“这个为期三年的项目强调EOVSA的独特能力，即通过动态测量日冕磁场沿着热电子和非热电子分布，以高空间和时间分辨率量化太阳耀斑的演变。 项目目标包括：（i）获得不断变化的日冕磁场和耀斑环中电子分布图;（ii）建立一致的不断变化的太阳耀斑三维模型，通过前向拟合，同时拟合所有现有数据，包括磁场、无线电、X射线、极紫外线和其他数据;以及（iii）向科学家和公众开放这些产品。 该项目小组将采用综合研究方法，将EOVSA提供的新微波成像数据、其他地面仪器（如有机会）提供的数据以及最新空间任务的数据结合起来，再加上先进的建模和前向拟合，以获得三维磁场和耀斑环中的粒子分布。 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。该奖项反映了NSF的法定使命，并通过使用基金会的知识价值和更广泛的影响审查标准进行评估，被认为值得支持。

Modern solar physics explores the Sun through new observations with fantastically improved spectral coverage and spatial, spectral, and temporal resolutions relative to only a few years ago, brought about by recent advances in technology. In parallel, the complexity and volume of the data have been increasing proportionally. The main goal of this three-year project is to tightly couple these multi-dimensional observations with theory, analysis tools, and modeling to obtain new knowledge and make fundamental scientific discoveries in solar physics, particularly about the nature of the physical drivers of the solar activity. The solar activity depends critically on coronal magnetism, which, broadly speaking, includes magnetic field generation, control of morphology/topology, temporal evolution, and transformation into kinetic, thermal, and non-thermal energies in the Sun's corona, as well as coupling between the magnetic and thermal structures. The ability to measure the coronal magnetic field and its changes on dynamic time scales is critically needed to uncover fundamental physics driving solar flares, eruptions, and activity. While reliable direct measurement of coronal magnetic fields has been lacking, this project aims to radically change the situation by taking full advantage of the large wealth of high resolution data and modeling that is finally becoming available. Specifically, a practical opportunity for routine use of radio observations of the Sun's corona for probing the magnetic structures involved in solar flares has recently become available for the first time from the new, fully functional microwave interferometer -- the NJIT's Expanded Owens Valley Solar Array (EOVSA) -- which has started regular interferometric observations of the Sun. To make sense of these highly demanding data, with progressively increasing volume and complexity, and to integrate these data into a full synthetic picture of the magnetic and thermal structure along with accelerated non-thermal electrons in solar flares, this project will utilize sophisticated models that combine the most advanced theories, computational codes, and simulation tools with the data.This project includes broad dissemination of the new knowledge gathered in solar radio-astronomy to enhance scientific understanding not only in solar physics, but also throughout astrophysics. The fundamental nature of EOVSA's observations ensures a broad impact on the field of solar physics, including future instrument development for the DIKIST, FASR, etc. The work will result in user-friendly software tools that will be made widely available to the solar and space weather community through the Solarsoft IDL distribution library. These modeling tools will be used during the summer internships at the NJIT's Center for Solar-Terrestrial Research (CSTR), where the project team recruits local junior high school students to participate in cutting-edge solar research. In addition, being performed within highly diverse environment provided by the CSTR at NJIT, the various project activities will advance discovery and understanding, while promoting teaching, training and learning. In particular, the easy-to-use tools to be developed during this project make great learning tools that will be widely used in graduate courses at the CSTR, such as "Radio Astronomy," "Solar Physics," and "Plasma Physics and MHD."The three-year project emphasizes the unique ability of EOVSA to quantify evolution of solar flares by dynamically measuring coronal magnetic fields along with the thermal and non-thermal electron distributions with high spatial and temporal resolution. The project objectives include: (i) obtain evolving maps of coronal magnetic field and electron distributions in the flaring loops; (ii) build consistent evolving three-dimensional models of solar flares that, through forward fitting, simultaneously fit all available data, including the magnetic field, radio, X-ray, EUV and others; and, (iii) provide open access to these product to the scientists and the public. The project team will adopt an integrated research approach that brings together new microwave imaging data available from the EOVSA, data from other ground-based instruments as opportunities allow, and data from the latest space missions, coupled with advanced modeling and forward-fitting, to obtain the three-dimensional magnetic field and particle distributions in flaring loops. The research and EPO agenda of this project supports the Strategic Goals of the AGS Division in discovery, learning, diversity, and interdisciplinary research.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.