SHINE: Magnetic Reconnection in Solar Eruptions

本研究的目的是观测研究磁重联在大规模太阳爆发和日冕物质抛射（cme）中的作用。为此，将对cme和太阳表面活动的观测数据进行广泛的数据分析，如太阳耀斑和细丝，这些数据将由地面设施（如大熊太阳天文台（BBSO）的全球Ha网络）和卫星任务（如LASCO， TRACE， RHESSI，以及SoHO上的EIT和MDI仪器）获得。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的表观运动和耀斑斑扫过的磁场，以评估日冕中磁重联的速率。物质抛射的动态演化将通过CME观测以及对喷发细丝和日冕结构的光学和极紫外观测来测量。将质量抛射早期质量加速度的时间分布与推断的磁重联率进行比较，以观测重联与加速度之间的时间相关性和幅度标度关系。我们将分析不同磁构型的太阳爆发事件，特别是喷发磁结构的逆和正构型，以检验在不同磁构型下重联-加速关系是否成立。通过观测测量磁重联的震级、持续时间、高度、磁重联传递的质量和磁通量、磁重联释放的磁能等与磁重联和磁环境相关的物理参数，研究磁重联对大尺度火山喷发动力学演化和能量学的影响。

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.