SHINE: Magnetic Reconnection in Solar Eruptions

SHINE：太阳喷发中的磁重联

• 批准号: 0454606
• 负责人: Jiong Qiu
• 金额: $ 3.61万
• 依托单位: New Jersey Institute of Technology
• 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: 2005-01-01 至 2006-01-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0454606&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.

拟议的研究的目的是观察磁重新连接在大规模太阳喷发和冠状质量弹出（CMES）中的作用。为此，将对CME和太阳表面的活动的观察结果进行广泛的数据分析，例如太阳耀斑和丝状，由基于地面的设施（例如Big Bear Solar Percervatory的全球HA网络（BBSO）（BBSO）和卫星任务，以及诸如Lasco，Trace，Trace，Trace，Rhessi，Rhessi和Eit和Mdi Instermutse和Mdi Instermutse offerionSter和Mdi Instermutse ins-soho-soho-soho-sohoho-soho-soho-sohoho-soho sohoho insoho sohoho sohoho sohoho soho insoho so.使用对HA，UV和EUV波长的观测，建议者将测量下部太阳大气中耀斑斑块的明显运动以及斑块扫描的磁场，以评估电晕中磁重新连接的速率。质量弹出的动态演变将使用CME观测值以及发射细丝和冠状结构的光学和EUV观测值测量。将质量加速度在质量喷射早期阶段的时间曲线与推断的磁重新连接速率进行比较，以观察重新连接与加速度之间的时间相关性和幅度缩放关系。将分析不同磁性构型的太阳喷发事件，特别是爆发磁性结构的逆配置和正常配置，以测试重新连接加速关系是否适用于不同的磁性构型。与磁重新连接和磁性环境相关的物理参数，例如通过磁重新连接传递的磁性重新连接的大小，持续时间和高度，以及通过磁重新连接释放的磁能，从观察值来研究磁重新连接对大型爆发的动态演化和能量的影响。