Ngampoopun Nawin, Susino Roberto, Brooks David H, Lionello Roberto, Abbo Lucia, Spadaro Daniele, Baker Deborah, Green Lucie M, Long David M, Yardley Stephanie L, James Alexander W, Romoli Marco, Giordano Silvio M, Burtovoi Aleksandr, Landini Federico, Russano Giuliana
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT UK.
National Institute for Astrophysics, Astrophysical Observatory of Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy.
Sol Phys. 2025;300(4):45. doi: 10.1007/s11207-025-02438-8. Epub 2025 Apr 3.
ESA/NASA's Solar Orbiter (SO) enables us to study the solar corona at closer distances and from different perspectives, which helps us to gain significant insights into the origin of the solar wind. In this work, we present the analysis of solar wind outflows from two locations: a narrow open-field corridor and a small, mid-latitude coronal hole. These outflows were observed off-limb by the Metis coronagraph onboard SO and on-disk by the Extreme Ultraviolet Imaging Spectrometer (EIS) onboard Hinode. Magnetic field extrapolations suggest that the upflow regions seen in EIS were the sources of the outflowing solar wind observed with Metis. We find that the plasma associated with the narrow open-field corridor has higher electron densities and lower outflow velocities compared to the coronal hole plasma in the middle corona, even though the plasma properties of the two source regions in the low corona are found to be relatively similar. The speed of the solar wind from the open-field corridor also shows no correlation with the magnetic field expansion factor, unlike the coronal hole. These pronounced differences at higher altitudes may arise from the dynamic nature of the low-middle corona, in which reconnection can readily occur and may play an important role in driving solar wind variability.
The online version contains supplementary material available at 10.1007/s11207-025-02438-8.
欧洲航天局/美国国家航空航天局的“太阳轨道飞行器”（Solar Orbiter，SO）使我们能够在更近的距离并从不同视角研究日冕，这有助于我们深入了解太阳风的起源。在这项工作中，我们展示了对来自两个位置的太阳风外流的分析：一个狭窄的开放磁场通道和一个小的中纬度日冕洞。这些外流由SO上的梅蒂斯日冕仪在日边缘外进行观测，并由日地关系天文台（Hinode）上的极紫外成像光谱仪（EIS）在日面上进行观测。磁场外推表明，EIS中观测到的上升流区域是用梅蒂斯观测到的外流太阳风的来源。我们发现，与中冕中的日冕洞等离子体相比，与狭窄开放磁场通道相关的等离子体具有更高的电子密度和更低的外流速度，尽管在低冕中两个源区的等离子体特性相对相似。与日冕洞不同，来自开放磁场通道的太阳风速度也与磁场膨胀因子没有相关性。在较高高度的这些显著差异可能源于低-中冕的动态性质，其中重联很容易发生，并且可能在驱动太阳风变化中起重要作用。
在线版本包含可在10.1007/s11207-025-02438-8获取的补充材料。
