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: 1839306
• 负责人: R. T. James McAteer
• 金额: $ 36.8万
• 依托单位: New Mexico State University
• 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 2024-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1839306&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.

在阳光下，在活跃和安静的大型结构中都发现了磁场，并从太阳表面爆发，称为太阳丝。研究人员建议制作和研究一个大型数据集，该数据集测量了这些细丝内部的磁场，包括活跃和安静的太阳丝，包括爆发和非喷发构型。这些研究将涵盖太阳丝的生命周期中的所有步骤，从形成到稳定到爆发。仅使用配备了特殊仪器的中型望远镜，现在才有可能获得研究太阳丝所需的完整磁场数据集。 调查人员将准备好研究新的Daniel K. Inouye Solar望远镜在开始运行时以更大决议制作的太阳丝的观察。 该项目通过促进我们对太阳的磁场结构和活动的理解来支持NSF的任务。研究人员将包括一名研究生和博士后助理，以支持研究并学习数据分析技术。磁性主义作为线性，剪切的结构，可以形成灯丝。结构中缺乏跨场漂移可以稳定热化和塌陷的细丝血浆。只有磁性才能快速重新排列结构并导致喷发。将解决三个特定的科学问题：形成太阳丝的磁场配置是什么？ 稳定太阳丝的磁场配置是什么？ 喷发前细丝的磁场配置是什么？ 为了解决这些问题，研究人员设定了三个特定的目标：在10830a的He I吸收线中定义并获得十个光谱序列，以研究灯丝形成。通过生产管道来减少，分析和解释这些光谱极化数据来对太阳丝结构进行分类。在失去细丝稳定性之前，识别那些磁性构型。数据分析要求对人员进行运行和扩展榛树倒置法规的培训，以研究磁性结构。该奖项反映了NSF的法定任务，并被认为是值得通过基金会的知识分子和更广泛影响的评估审查标准来通过评估来支持的。

项目成果

Velocities of an Erupting Filament

喷发细丝的速度

• DOI: 10.3847/1538-4357/ac3a04
• 发表时间: 2022
• 期刊: The Astrophysical Journal
• 作者: Wang, Shuo;Jenkins, Jack M.;Muglach, Karin;Martinez Pillet, Valentin;Beck, Christian;Long, David M.;Choudhary, Debi Prasad;McAteer, James
• 通讯作者: McAteer, James

Magnetic Structure of an Erupting Filament

喷发细丝的磁性结构

• DOI: 10.3847/1538-4357/ab7380
• 发表时间: 2020
• 期刊: The Astrophysical Journal
• 作者: Wang, Shuo;Jenkins, Jack M.;Martinez Pillet, Valentin;Beck, Christian;Long, David M.;Prasad Choudhary, Debi;Muglach, Karin;McAteer, James
• 通讯作者: McAteer, James