论文标题
跟踪从太阳到地球的磁通量和螺旋性 - 磁性云及其太阳能源的多间谍分析
Tracking magnetic flux and helicity from Sun to Earth -- Multi-spacecraft analysis of a magnetic cloud and its solar source
论文作者
论文摘要
我们分析了由太阳喷发事件引起的完整效应链，以便更好地了解行星际空间中磁场相关量的动态演化，尤其是磁通量和螺旋性。 We study a series of connected events (a confined C4.5 flare, a flare-less filament eruption and a double-peak M-class flare) that originated in NOAA active region (AR) 12891 on 2021 November 1 and November 2. We deduce the magnetic structure of AR 12891 using stereoscopy and nonlinear force-free (NLFF) magnetic field modeling, allowing us to identify a coronal flux rope and to estimate它的轴向通量和螺旋。此外，我们根据遥感图像的耀斑色带和冠状色调标志来计算重新连接通量。与相应数量的磁云（MC）相比，是根据太阳轨道和近地太空飞船的原位测量得出的，使我们能够对相关星际冠状质量射血（ICME）的演变得出结论。后者通过将几何拟合技术（渐变的圆柱形壳建模； GC）和行星际传播模型（基于阻力的集合建模； DBEM）应用于ICME来帮助后者。 NLFF建模表明，左手（负（负）剪切座椅/通量绳的形式，宿主AR的磁性结构达到了光泽水平以上8-10 mm的高度，与相应的立体镜估计密切一致。从GCS和DBEM建模中揭示，弹出的通量绳索以自相似的扩展方式通过星际空间传播。太阳能源区域中磁重新连接处理的磁通量和螺旋性的比较以及MC的各个预算表明，喷发前的预算也有相当大的贡献。
We analyze the complete chain of effects caused by a solar eruptive event in order to better understand the dynamic evolution of magnetic-field related quantities in interplanetary space, in particular that of magnetic flux and helicity. We study a series of connected events (a confined C4.5 flare, a flare-less filament eruption and a double-peak M-class flare) that originated in NOAA active region (AR) 12891 on 2021 November 1 and November 2. We deduce the magnetic structure of AR 12891 using stereoscopy and nonlinear force-free (NLFF) magnetic field modeling, allowing us to identify a coronal flux rope and to estimate its axial flux and helicity. Additionally, we compute reconnection fluxes based on flare ribbon and coronal dimming signatures from remote sensing imagery. Comparison to corresponding quantities of the associated magnetic cloud (MC), deduced from in-situ measurements from Solar Orbiter and near-Earth spacecraft, allows us to draw conclusions on the evolution of the associated interplanetary coronal mass ejection (ICME). The latter are aided through the application of geometric fitting techniques (graduated cylindrical shell modeling; GCS) and interplanetary propagation models (drag based ensemble modeling; DBEM) to the ICME. NLFF modeling suggests the host AR's magnetic structure in the form of a left-handed (negative-helicity) sheared arcade/flux rope reaching to altitudes of 8-10 Mm above photospheric levels, in close agreement with the corresponding stereoscopic estimate. Revealed from GCS and DBEM modeling, the ejected flux rope propagated in a self-similar expanding manner through interplanetary space. Comparison of magnetic fluxes and helicities processed by magnetic reconnection in the solar source region and the respective budgets of the MC indicate a considerable contribution from the eruptive process, though the pre-eruptive budgets appear of relevance too.
