Collaborative Research: Enabling a strong DKIST start - The Magnetic Structure of Solar Filaments

合作研究：实现 DKIST 的强劲启动 - 太阳能细丝的磁结构

• 批准号: 1839334
• 负责人: Hao Sheng Lin
• 金额: $ 12.3万
• 依托单位: University of Hawaii
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2018
• 资助国家: 美国
• 起止时间: 2018-09-15 至 2022-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1839334&HistoricalAwards=false
• 关键词: Collaborative; Research; Enabling; strong; DKIST

On the Sun, magnetic fields are found in both active and quiet large structures forming and erupting from the Sun's surface called solar filaments. The investigators propose to make and study a large data set that measures the magnetic field inside these filaments, including both erupting and non-erupting configurations, of both active and quiet solar filaments. These studies will cover all steps in a solar filament's lifetime, from formation to stability to eruption. Obtaining the complete magnetic field data set required to study solar filaments is only now possible using a medium-sized telescope equipped with special instrumentation, now available to the investigators. The investigators will be ready to study observations of the solar filaments made at greater resolutions by the new Daniel K. Inouye Solar Telescope when it begins operation. This project supports the mission of the NSF by promoting our understanding of magnetic field structure and activity at the Sun. The investigators will include a graduate student and a post-doctoral associate to support the research and learn data analysis techniques.Magnetism exists as linear, sheared structures that allows for filament formation; the lack of cross-field drift in the structure stabilizes the filament plasma from thermalization and collapse; and only magnetism can rapidly rearrange structure and result in eruption. Three specific science questions will be addressed: What is the magnetic field configuration of forming solar filaments? What is the magnetic field configuration of stable solar filaments? What is the magnetic field configuration of a filament prior to eruption? To address these, the investigators set three specific objectives: Define and obtain ten spectropolarimetric sequences in the He I absorption line at 10830A, in order to study filament formation. Classify solar filament structure by producing a pipeline to reduce, analyze, and interpret these spectropolarimetric data. Identify those magnetic configurations prior to a loss of filament stability. Data analysis requires the training of personnel in running and expanding the HAZEL inversion code into pipeline in order to study the magnetic structure.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.

在太阳上，磁场存在于活跃和安静的大型结构中，这些结构从太阳表面形成和爆发，称为太阳细丝。研究人员建议制作和研究一个大型数据集，测量这些丝状体内部的磁场，包括活跃和安静的太阳丝状体的爆发和非爆发配置。这些研究将涵盖太阳灯丝生命周期的所有步骤，从形成到稳定再到爆发。获得研究太阳细丝所需的完整磁场数据集现在只有使用配备特殊仪器的中型望远镜才有可能，现在可供研究人员使用。 研究人员将准备研究新的丹尼尔K。Inouye太阳望远镜开始运行时。 该项目通过促进我们对太阳磁场结构和活动的理解来支持NSF的使命。研究人员将包括一名研究生和一名博士后助理，以支持研究和学习数据分析技术。磁性以线性剪切结构存在，允许细丝形成;结构中缺乏交叉场漂移使细丝等离子体稳定，不受热化和塌陷的影响;只有磁性才能迅速重新排列结构并导致爆发。三个具体的科学问题将得到解决：什么是形成太阳灯丝的磁场配置？ 稳定的太阳暗条的磁场结构是什么？ 在爆发之前，暗条的磁场结构是怎样的？ 为了解决这些问题，研究人员设定了三个具体目标：定义并获得He I吸收线10830 A处的十个光谱偏振序列，以研究细丝的形成。分类太阳能灯丝结构通过生产一个管道，以减少，分析和解释这些光谱偏振数据。在灯丝稳定性丧失之前识别这些磁配置。数据分析需要培训人员在管道中运行和扩展HAZEL反演代码，以研究磁结构。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。