Collaborative Research: SHINE--Using Photospheric Imprints of Coronal Currents to Understand Coronal Magnetic Structure

合作研究：SHINE——利用日冕电流的光球印记来了解日冕磁结构

• 批准号: 2302697
• 负责人: Brian Welsch
• 金额: $ 14.45万
• 依托单位: University of Wisconsin-Green Bay
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2023
• 资助国家: 美国
• 起止时间: 2023-06-01 至 2026-05-31
• 项目状态: 未结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=2302697&HistoricalAwards=false
• 关键词: Collaborative; Research; SHINE; Using; Photospheric

Solar flares and coronal mass ejections (CMEs) drive the strongest disturbances in the solar system. These events are powered by the sudden release of magnetic energy stored in electric currents flowing in the coronal magnetic field. Basic questions about these currents remain: How do coronal currents evolve to become unstable in the lead up to such events? And how do these currents evolve to release magnetic energy during flares and CMEs? This project addresses these questions through modeling and analysis of coronal extreme ultra violet (EUV) images. The broader impacts include mentoring of undergraduate students and collaboration between US and Australian institutes. Outreach will be conducted for the Great American October 2023 and April 2024 solar eclipses. This project will employ Gauss’s separation method — which has a long heritage in terrestrial and planetary magnetism — to photospheric vector magnetograms (2D maps of the 3-component magnetic field) of solar active regions (ARs). The core idea of Gauss’s method is that the photospheric field can be unambiguously partitioned into three distinct parts, each with its own source: currents below the photosphere, currents above it, and currents passing through it. We refer to the part of the photospheric field due to coronal currents as the ”photospheric imprint” of these currents. Photospheric imprints, by themselves, cannot fully reveal the nature of coronal currents. Nonlinear, force-free field (NLFFF) extrapolations have previously been used to study coronal currents, but fields on these models’ bottom boundaries typically exhibit substantial inconsistencies with magnetogram fields. While both methods have limitations, combining them can substantially improve our under- standing of coronal currents. Accordingly, the project will exploit both approaches in case studies of flare- and CME-prone ARs, to investigate the structure and development of coronal currents. The team will analyze evolution in photospheric imprints and NLFFF models before and after flares/CMEs, and in quiet epochs to establish baseline rates of change. Coronal EUV images will also be studied for context.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.

太阳耀斑和日冕物质抛射（CME）是太阳系中最强烈的扰动。这些事件是由储存在日冕磁场中流动的电流中的磁能突然释放提供动力的。关于这些电流的基本问题仍然存在：日冕电流是如何演变成不稳定的，从而导致这些事件的发生的？在耀斑和日冕物质抛射期间，这些电流是如何演变以释放磁能的？该项目通过对日冕极紫外（EUV）图像的建模和分析来解决这些问题。更广泛的影响包括对本科生的指导以及美国和澳大利亚机构之间的合作。将为2023年10月和2024年4月的大美国日食进行宣传。该项目将采用高斯的分离方法-该方法在地磁学和行星磁学方面有着悠久的历史-来绘制太阳活动区的光球矢量磁图（三分量磁场的二维地图）。高斯方法的核心思想是，光球场可以明确地划分为三个不同的部分，每个部分都有自己的来源：光球下方的电流，光球上方的电流，以及穿过光球的电流。我们将日冕电流引起的光球场部分称为这些电流的“光球印记”。光球印记本身并不能完全揭示日冕电流的本质。非线性无力场（NLFFF）外推法此前曾用于研究日冕电流，但这些模型底部边界上的场通常与磁图场表现出实质性的不一致。虽然这两种方法都有局限性，但将它们结合起来可以大大提高我们对日冕电流的理解。因此，该项目将在易发生耀斑和日冕物质抛射的AR案例研究中利用这两种方法，以调查日冕电流的结构和发展。该团队将分析耀斑/CME前后光球印记和NLFFF模型的演变，以及安静时期的演变，以建立基线变化率。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。