2025-11-10 中国科学院（CAS）
Figure 1. (a) Distribution of the sunspot and the jets analyzed in this study. The umbra is marked in black and the penumbra in white. The colors of the jets indicate the projected velocities. (b)–(e) Histograms comparing the velocity, length, width, and lifetime of the jets. Inside jets are shown in red, while outside jets are shown in blue. The dashed lines mark the mean values of each group. (Image by WU Guotang)
＜関連情報＞
- https://english.cas.cn/newsroom/research_news/phys/202511/t20251111_1098092.shtml
- https://iopscience.iop.org/article/10.3847/1538-4357/ae1198
NVSTとSDOによる太陽黒点周辺の彩層ジェットの観測研究 Observational Study of Chromospheric Jets In and Around a Sunspot Observed by NVST and SDO
Guotang Wu, Xiaoli Yan, Zhike Xue, Jincheng Wang, Zhe Xu, Liheng Yang, Yian Zhou, Liping Yang, Xinsheng Zhang, Qifan Dong,…
The Astrophysical Journal Published: 2025 October 31
DOI:10.3847/1538-4357/ae1198
Abstract
To better understand the characteristics, driving mechanisms, and potential heating contributions of chromospheric jets, we analyze two contrasting types: one originating from within the sunspot penumbra (inside jets) and the other originating from outside the penumbra (outside jets). Statistical analysis of 100 jets (50 inside jets and 50 outside jets) reveals that inside jets have a projected velocity range of 4–14 km s−1, a length range of 1–4 Mm, a width range of 0.2–0.6 Mm, and a lifetime range of 135–450 s, with mean values of 7.90 km s−1, 2.61 Mm, 0.41 Mm, and 260 s, respectively. About 52% of inside jets are associated with brightenings in Hα blue wing images, and some show high-temperature signatures, suggesting a connection with localized energy release. In contrast, outside jets have higher velocities (8–50 km s−1, average 19.04 km s−1), greater lengths (average 6.26 Mm, up to 27.27 Mm), slightly larger widths (average 0.46 Mm), and longer lifetimes (135–630 s, average 327 s). They typically originate from regions of opposite magnetic polarities and are associated with magnetic flux emergence and extreme-ultraviolet brightenings. Some outside jets correspond to coronal jets with inverted Y-shaped structures and temperatures exceeding one million Kelvin. Our results suggest that both jet types are driven by magnetic reconnection occurring in distinct magnetic field configurations and contribute to chromospheric and coronal heating.
