SHINE: Magnetic Reconnection in Solar Eruptions

SHINE：太阳喷发中的磁重联

• 批准号: 0603789
• 负责人: Jiong Qiu
• 金额: --
• 依托单位: Montana State University
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2005
• 资助国家: 美国
• 起止时间: 2005-10-21 至 2008-06-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0603789&HistoricalAwards=false
• 关键词: SHINE; Magnetic; Reconnection; Solar; Eruptions

The objective of the proposed research is to observationally study the role of magnetic reconnection in large-scale solar eruptions and Coronal Mass Ejections (CMEs). To this end, extensive data analysis will be conducted on observations of CMEs and activity on the Sun's surface, such as solar flares and filaments, obtained by both ground-based facilities, such as the Global Ha Network at Big Bear Solar Observatory (BBSO), and satellite missions, such as LASCO, TRACE, RHESSI, and the EIT and MDI instruments on-board SoHO. Using observations at Ha, UV, and EUV wavelengths, the proposers will measure the apparent motion of flare patches in the lower solar atmosphere and the magnetic fields that the patches sweep through, to evaluate the rate of magnetic reconnection in the corona. The dynamic evolution of mass ejections will be measured using CME observations, as well as optical and EUV observations, of eruptive filaments and coronal structures. The time profiles of mass acceleration at the early stage of mass ejection will be compared with the inferred magnetic reconnection rate to observationally examine the temporal correlation and magnitude scaling relationship between reconnection and acceleration. Solar eruptive events of different magnetic configurations, specifically the inverse and normal configurations of the erupting magnetic structure, will be analyzed to test whether the reconnection-acceleration relationship holds for different magnetic configurations. Physical parameters relevant to magnetic reconnection and magnetic environment, such as the magnitude, duration, and height of magnetic reconnection, mass and magnetic flux transferred by magnetic reconnection, and magnetic energy released through magnetic reconnection, will be measured from observations to study the impact of magnetic reconnection on the dynamical evolution and energetics of large-scale eruptions.

拟议研究的目的是观测研究磁重联在大规模太阳喷发和日冕物质抛射（CME）中的作用。为此，将对日冕物质抛射和太阳表面活动（例如太阳耀斑和灯丝）的观测进行广泛的数据分析，这些数据是由大熊太阳天文台（BBSO）的全球哈网络等地面设施获得的，以及卫星任务，例如 LASCO、TRACE、RHESSI 以及 SoHO 上的 EIT 和 MDI 仪器。利用 Ha、UV 和 EUV 波长的观测，提议者将测量太阳低层大气中耀斑斑块的视运动以及耀斑斑块扫过的磁场，以评估日冕中磁重联的速率。质量抛射的动态演化将使用日冕物质抛射观测以及喷发丝和日冕结构的光学和极紫外观测来测量。将质量抛射早期的质量加速度的时间分布与推断的磁重联率进行比较，以观察性地检查重联和加速度之间的时间相关性和幅度缩放关系。将分析不同磁配置的太阳喷发事件，特别是喷发磁结构的逆配置和正配置，以测试重联-加速关系是否适用于不同的磁配置。通过观测测量与磁重联和磁环境相关的物理参数，例如磁重联的大小、持续时间和高度、磁重联传递的质量和磁通量以及磁重联释放的磁能，以研究磁重联的影响。磁重联对大规模喷发的动力学演化和​​能量学的影响。