Ubiquitous Small-scale EUV Upflow-Like Events above Network Regions Observed by the Solar Orbiter/Extreme Ultraviolet Imager
Fuente:
arXiv
Enregistré dans:
| Auteurs principaux: | , , , , |
|---|---|
| Format: | Preprint |
| Publié: |
2024
|
| Sujets: | |
| Accès en ligne: | |
| Tags: |
Ajouter un tag
Pas de tags, Soyez le premier à ajouter un tag!
|
| _version_ | 1866916529554063360 |
|---|---|
| author | Duan, Yadan Chen, Hechao Hou, Zhenyong Sun, Zheng Shen, Yuandeng |
| author_facet | Duan, Yadan Chen, Hechao Hou, Zhenyong Sun, Zheng Shen, Yuandeng |
| contents | Universal small-scale solar activity in quiet region are suggested to be a potential source of solar wind and the upper solar atmosphere. Here, with the high-resoltion 174 Å~imaging observations from the Solar Orbiter/Extreme Ultraviolet Imager (EUI), we investigate 59 EUV upflow-like events observed in the quiet Sun. Their average apparent (plane-of-sky) velocity, lifetime, and propagation distance are measured as 62 $\speed$, 68.6 s and 3.94 Mm, respectively. These upflow-like events exhibit dynamic characteristics but lack base brightening, featuring a hot front and subsequent cold plasma ejection. 39\% of the EUV upflow-like events exhibit recurrent characteristics. Unprecedented high-resolution 174 Å~observations reveal that some EUV upflow-like events exhibit blob-like fine structures and multi-strand evolutionary features, and some upflow-like events can cause localized haze-like plasma heating ahead of their spire region during the ejection process. A subset of the EUV upflow-like events covered by the Solar Dynamics Observatory reveals that they appear at the chromospheric networks. Through emission measure analysis, we found that these upflow-like events eject hot plasma of transient region or coronal temperature (an average of $\sim$10$^{5.5}$K). We suggest that EUV upflow-like events may be EUV counterparts of chromospheric spicules and/or transition region network jets, and play a role in heating localized corona above the network regions. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2412_13444 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Ubiquitous Small-scale EUV Upflow-Like Events above Network Regions Observed by the Solar Orbiter/Extreme Ultraviolet Imager Duan, Yadan Chen, Hechao Hou, Zhenyong Sun, Zheng Shen, Yuandeng Solar and Stellar Astrophysics Universal small-scale solar activity in quiet region are suggested to be a potential source of solar wind and the upper solar atmosphere. Here, with the high-resoltion 174 Å~imaging observations from the Solar Orbiter/Extreme Ultraviolet Imager (EUI), we investigate 59 EUV upflow-like events observed in the quiet Sun. Their average apparent (plane-of-sky) velocity, lifetime, and propagation distance are measured as 62 $\speed$, 68.6 s and 3.94 Mm, respectively. These upflow-like events exhibit dynamic characteristics but lack base brightening, featuring a hot front and subsequent cold plasma ejection. 39\% of the EUV upflow-like events exhibit recurrent characteristics. Unprecedented high-resolution 174 Å~observations reveal that some EUV upflow-like events exhibit blob-like fine structures and multi-strand evolutionary features, and some upflow-like events can cause localized haze-like plasma heating ahead of their spire region during the ejection process. A subset of the EUV upflow-like events covered by the Solar Dynamics Observatory reveals that they appear at the chromospheric networks. Through emission measure analysis, we found that these upflow-like events eject hot plasma of transient region or coronal temperature (an average of $\sim$10$^{5.5}$K). We suggest that EUV upflow-like events may be EUV counterparts of chromospheric spicules and/or transition region network jets, and play a role in heating localized corona above the network regions. |
| title | Ubiquitous Small-scale EUV Upflow-Like Events above Network Regions Observed by the Solar Orbiter/Extreme Ultraviolet Imager |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2412.13444 |