SHINE: Physics-based and Statistical Studies Connecting Surface-field Distributions to the Magnetic Flux Rope Structure in the Corona and Heliosphere

SHINE：基于物理和统计的研究将表面场分布与日冕和日光层的磁通绳结构联系起来

• 批准号: 2228967
• 负责人: Hong Xie
• 金额: $ 50.85万
• 依托单位: Catholic University of America
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2022
• 资助国家: 美国
• 起止时间: 2022-11-01 至 2025-10-31
• 项目状态: 未结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=2228967&HistoricalAwards=false
• 关键词: SHINE; Physics; based; Statistical; Studies

Coronal mass ejections (CMEs) from the Sun are the driver of extreme space weather near Earth. This project addresses the Solar, Heliospheric, and Interplanetary Environment (SHINE) goal of understanding the origin and evolution of CMEs through an investigation of magnetic flux ropes. The project is led by scientists from under-represented groups in STEM, who will mentor undergraduate students from underrepresented ethnic minority groups or first-generation college students. The project advances the participation of women in science. Outreach will also be conducted in preparation for the October 2023 and April 2024 solar eclipses.The central goal of this project is to obtain a quantitative understanding of the structure and evolution of magnetic flux ropes from the solar photosphere to the inner heliosphere. The scientific objective of the work is to determine how the reconnected magnetic flux in the solar source region drives the CME flux rope structure in the corona and heliosphere. The proposed objective will be achieved by answering the questions: 1) Do flux ropes exist prior to eruptions, or are they formed during eruptions, or some combination of the two? 2) How magnetic reconnection affect the magnetic properties and kinematics of CME flux ropes? A combination of photospheric and coronal observations combined with flux rope fitting form the basis for geometrical and magnetic characterization of the “flux rope from eruption data” (FRED). The team will determine the direction of the axial magnetic field and magnetic flux rope (MFR) helicity by a combination of magnetogram data and EUV eruptive features (e.g., coronal arcade skews, Fe XII stalks, sigmoids, and magnetic tongues) in solar source regions. Since the flux rope legs are anchored in the photosphere within the EUV core dimming regions in the eruption site, the magnetic flux within the core dimming region corresponds to the flux rope’s axial flux. The reconnected flux within the post eruption arcade corresponds to the poloidal flux of the flux rope. Thus, a MFR is fully defined in the corona and its evolution is tracked under the assumption of self-similar expansion, enabling the prediction of the Bz (out of the ecliptic field) component that encounters Earth. The coronal flux rope structure will be compared against the flux rope in the heliosphere fitted to in-situ observations at various heliocentric distances (Parker Solar Probe, Solar Orbiter, and spacecraft near 1 AU), including self-similar expansion, helicity and the orientation of the coronal and interplanetary flux ropes. The team will use the elliptical flux rope and graduated cylindrical shell techniques for forward modeling of the CME flux ropes. Both the Lepping cylindrical force-free magnetic cloud fitting and Marubashi cylinder and torus fitting are used to derive the MFR structure in CMEs.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.

来自太阳的冠状质量弹出（CME）是地球附近极端天气的驱动力。该项目通过研究磁通绳来理解CME的起源和演变的太阳能，地球和星际环境（Shine）的目标。该项目由STEM中代表性不足的群体的科学家领导，他们将来自代表性不足的少数民族或第一代大学生的精神本科生。该项目推动了妇女参与科学的参与。还将进行外展活动，以准备2023年10月和2024年4月的太阳能日食。该项目的核心目标是对磁通绳从太阳能光球到内层的结构和演变进行定量理解。这项工作的科学目标是确定太阳能源区域中重新连接的磁通量如何驱动电晕和地球层中的CME通量绳结构。提出的目标将通过回答问题来实现：1）爆发前是否存在通量绳，还是在喷发期间形成，还是两者的某种组合？ 2）磁重新连接如何影响CME通量绳索的磁性和运动学？光球和冠状观测与通量绳拟合结合的结合构成了“喷发数据中的通量绳”（FRED）的几何和磁性表征的基础。该团队将通过磁力图数据和EUV喷发特征（例如，冠状街道偏斜，Fe XII茎，Sigmoids和Magement Tongues）在太阳能源区域确定轴向磁场和磁通绳（MFR）螺旋的方向。由于通量绳腿固定在喷发部位的EUV核心调光区域内的光球中，因此核心调光区域内的磁通量对应于磁通绳的轴向通量。爆发后拱廊内的重新连接通量对应于通量绳的poloidal通量。这是在电晕中完全定义的MFR，并且在自相似扩张的假设下跟踪其演变，从而实现了遇到地球的BZ（超出黄道场）组件的预测。将在各种地中心距离（Parker Solar Probe，Solar Orbiter，太阳能轨道和1 AU的航天器）（包括自相似的膨胀，Helicition，Helicition，Helicition and Helicition及其冠状动脉和冠状动脉圈型冠状动脉和室内劳动力的方向）中，将比较冠状绳绳结构与适合于原位观测的地球层的通量绳相比。该团队将使用椭圆通量的绳索和渐变的圆柱壳技术来进行CME通量绳的正向建模。 Lepping圆柱形无力的磁云配件以及Marubashi圆柱体和圆环拟合都用于得出CMES中的MFR结构。该奖项反映了NSF的法定任务，并通过使用基金会的知识分子优点和更广泛的影响审查标准来评估通过评估来诚实地支持。

项目成果

What Do Halo CMEs Tell Us about Solar Cycle 25?

关于太阳周期 25，Halo 日冕物质抛射告诉我们什么？

• DOI: 10.3847/2041-8213/acdde2
• 发表时间: 2023
• 期刊: The Astrophysical Journal Letters
• 作者: Gopalswamy, Nat;Michalek, Grzegorz;Yashiro, Seiji;Mäkelä, Pertti;Akiyama, Sachiko;Xie, Hong
• 通讯作者: Xie, Hong