SHINE: Magnetic Reconnection in Solar Eruptions

拟议研究的目的是从观测角度研究磁场重联在大规模太阳喷发和日冕物质抛射中的作用。为此目的，将对日冕物质系统和太阳表面活动的观测结果进行广泛的数据分析，这些观测数据是由地面设施，如大熊太阳天文台的全球太阳活动网络，以及卫星飞行任务，如LASCO、TRACE、RHESSI和SOHO上的EIT和计量吸入器获得的。利用在Ha、UV和EUV波长的观测，提出者将测量较低太阳大气中耀斑的表观运动以及这些斑块扫过的磁场，以评估日冕中的磁重联速度。将使用CME观测以及喷发细丝和日冕结构的光学和EUV观测来测量物质抛射的动态演变。将质量抛射早期的质量加速时间分布与所推算的磁重联率进行比较，以观测到重联和加速之间的时间相关性和星等标度关系。将分析不同磁构型的太阳喷发事件，特别是喷发磁结构的逆构型和正常构型，以测试重联-加速关系是否适用于不同的磁构型。与磁重联和磁环境有关的物理参数，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，将从观测中测量，以研究磁重联对大规模喷发的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.