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

在太阳上，活跃的和安静的大型结构中都有磁场，这些结构从太阳表面形成并喷发，称为太阳丝。研究人员提议制作和研究一个大型数据集，测量这些细丝内部的磁场，包括活动和静止太阳细丝的喷发和非喷发配置。这些研究将涵盖太阳细丝寿命的所有阶段，从形成到稳定再到爆发。现在只有使用配备了特殊仪器的中型望远镜才能获得研究太阳细丝所需的完整磁场数据集，研究人员现在可以使用这种望远镜。研究人员将准备好研究新的丹尼尔·K·井上太阳望远镜在更高分辨率下对太阳细丝的观测，当它开始运行时。该项目通过促进我们对太阳磁场结构和活动的了解来支持国家科学基金会的任务。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、剪切结构的形式存在，允许细丝形成；结构中没有跨场漂移，稳定了细丝等离子体，使其免受热化和崩塌；只有磁性才能迅速重新排列结构并导致喷发。三个具体的科学问题将被解决：形成太阳细丝的磁场配置是什么？稳定的太阳细丝的磁场构型是什么？细丝在喷发前的磁场构型是什么？为了解决这些问题，研究人员设定了三个具体的目标：定义并获得10830A的He-I吸收线上的十个偏振光谱序列，以便研究灯丝的形成。通过制作一条管道来对太阳灯丝结构进行分类，以减少、分析和解释这些光谱偏振数据。在灯丝失去稳定性之前确定这些磁性配置。数据分析需要培训人员运行和扩展到管道中，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。

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.