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| Main Authors: | , , , |
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| Format: | Preprint |
| Published: |
2025
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2502.12889 |
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Table of Contents:
- We use data from the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) to study the most likely formation of a forced reconnection region and associated plasma blobs, triggered by jet-like structures in a prominence segment. Around 05:44 UT on December 16$^{th}$, 2017, hot jet-like structures lifted from a nearby active region and fell obliquely on one side of the prominence segment with velocities of $\approx$45--65 km s$^{-1}$. These eruptions compressed the boundaries of the prominence and flux rope, forming an elongated reconnection region with inflow velocities of 47--52 km s$^{-1}$ and 36--49 km s$^{-1}$ in the projected plane. A thin, elongated reconnection region was formed, with multiple magnetic plasma blobs propagating bidirectionally at velocities of 91--178 km s$^{-1}$. These dense blobs, associated with ongoing reconnection, may also be linked to the onset of Kelvin-Helmholtz (K-H) instability. The blobs are attributed to plasmoids, moving at slower speeds (91--178 km s$^{-1}$) due to the high density in the prominence segment. The dimensionless reconnection rate varied from 0.57--0.28, 0.53--0.26, and 0.41--0.20, indicating reconnection rate enhancement and supporting the forced reconnection scenario. After reconnection, the prominence plasma heated to 6 MK, releasing significant thermal energy ($\approx$5.4$\times$10$^{27}$ erg), which drained cool prominence plasma and heated it to coronal temperatures. The ubiquity of jets and outflows in the solar atmosphere makes the aforementioned of reconnection and possible co-existence of K-H instability potentially important for the magnetic energy release and heating in the solar atmosphere.