A Novel and Powerful Way to Measure Coronal Magnetic Fields for the DKIST Era

DKIST 时代测量日冕磁场的新颖而强大的方法

• 批准号: 1725247
• 负责人: Jeffrey Kuhn
• 金额: $ 32.94万
• 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: 2017
• 资助国家: 美国
• 起止时间: 2017-08-15 至 2024-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1725247&HistoricalAwards=false
• 关键词: Novel; Powerful; Way; Measure; Coronal

One of the major unsolved problems in solar physics is the question regarding how the solar corona is heated to temperatures over a million degrees. This project will develop and install new instrumentation on the institution's Scatter-free Observatory for Limb, Active Regions and Coronae (SOLARC) telescope. This instrumentation will operate in the infrared and will take advantage of a new approach to observing weak emission lines in the corona. These measurements will be used to derive the magnetic fields in the corona which will, in turn, be compared to existing numerical models that predict coronal heating. This project will support the training of the next generation of solar scientists. The PI will involve a postdoctoral researcher in the project and also plans to incorporate summer interns on the graduate and undergraduate level. In this project, the PI will construct a new instrument to be installed on the SOLARC telescope. This new instrument will take advantage of a novel approach that is based on permitted-forbidden line pairs and the Hanle effect, which has two significant advantages over previous techniques. First, it only relies on measuring linearly polarized emission signals which are typically two (or more) orders of magnitude larger than previously used circularly polarized emission lines. Second, it uses emission lines at longer infrared (IR) wavelengths where the scattered light from Earth's atmosphere is greatly reduced. The observed coronal vector magnetic fields will then be compared to magnetohydrodynamic (MHD) models to better understand the heating mechanisms within the corona. The development effort should also provide a powerful method that can be applied directly to the high spatial resolution capabilities of the Daniel K. Inouye Solar Telescope's (DKIST's) IR instruments.

太阳物理学中一个尚未解决的主要问题是日冕如何被加热到超过一百万度的温度。 该项目将在该机构的无散射临边、活动区和日冕观测台（SOLARC）望远镜上开发和安装新仪器。 该仪器将在红外线下工作，并将利用一种新的方法来观测日冕中的弱发射线。 这些测量结果将用于导出日冕中的磁场，反过来，将其与预测日冕加热的现有数值模型进行比较。 该项目将支持培训下一代太阳科学家。 PI将在该项目中涉及一名博士后研究员，并计划在研究生和本科生层面纳入暑期实习生。在这个项目中，PI将建造一个新的仪器安装在SOLARC望远镜上。 这种新仪器将利用一种新的方法，该方法基于禁用线对和汉勒效应，与以前的技术相比，该方法具有两个显著的优势。 首先，它仅依赖于测量线性偏振发射信号，该线性偏振发射信号通常比先前使用的圆偏振发射线大两个（或更多）数量级。 其次，它使用较长红外（IR）波长的发射线，其中来自地球大气的散射光大大减少。 然后将观测到的日冕矢量磁场与磁流体动力学（MHD）模型进行比较，以更好地了解日冕内的加热机制。 开发工作还应该提供一种强大的方法，可以直接应用于丹尼尔K的高空间分辨率能力。Inouye Solar Telescope（DKIST）的红外仪器。