SHINE: Magnetic Reconnection in Solar Eruptions

拟议研究的目标是观测研究磁场重联在大规模太阳爆发和日冕物质抛射（CME）中的作用。为此目的，将对由地面设施，如大熊太阳观测站的全球Ha网络和卫星飞行任务，如LASCO、TRACE、RHESSI以及SoHO上的EIT和MDI仪器获得的日冕物质抛射和太阳表面活动，如太阳耀斑和丝状体的观测数据进行广泛的分析。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表观运动以及斑块扫过的磁场，以评估日冕中的磁重联率。将利用日冕物质抛射观测以及光学和极紫外线观测来测量物质抛射的动态演变。在物质抛射的早期阶段的质量加速度的时间分布将与推断的磁场重联率进行比较，以观测检查重联和加速度之间的时间相关性和幅度标度关系。将分析不同磁位形的太阳爆发事件，特别是爆发磁结构的逆位形和正位形，以测试重联-加速关系是否适用于不同的磁位形。将通过观测测量与磁场重联和磁环境有关的物理参数，例如磁场重联的幅度、持续时间和高度、磁场重联转移的质量和磁通量以及磁场重联释放的磁能，以研究磁场重联对大规模喷发的动力学演变和能量学的影响。

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.