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  Coronal Microjets in Quiet-Sun Regions Observed with the Extreme Ultraviolet Imager on Board the Solar Orbiter

Hou, Z., Tian, H., Berghmans, D., Chen, H., Teriaca, L., Schühle, U., et al. (2021). Coronal Microjets in Quiet-Sun Regions Observed with the Extreme Ultraviolet Imager on Board the Solar Orbiter. Astrophysical Journal, Letters, 918(1): L20. doi:10.3847/2041-8213/ac1f30.

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 Creators:
Hou, Zhenyong, Author
Tian, Hui, Author
Berghmans, David, Author
Chen, Hechao, Author
Teriaca, Luca1, Author           
Schühle, Udo1, Author           
Gao, Yuhang, Author
Chen, Yajie, Author
He, Jiansen, Author
Wang, Linghua, Author
Bai, Xianyong, Author
Affiliations:
1Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832289              

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Free keywords: Quiet sun; Solar ultraviolet emission; Solar corona
 Abstract: We report the smallest coronal jets ever observed in the quiet Sun with recent high-resolution observations from the High Resolution Telescopes (HRIEUV and HRILyα) of the Extreme Ultraviolet Imager on board the Solar Orbiter (SO). In the HRIEUV (174 Å) images, these microjets usually appear as nearly collimated structures with brightenings at their footpoints. Their average lifetime, projected speed, width, and maximum length are 4.6 minutes, 62 km s−1, 1.0 Mm, and 7.7 Mm, respectively. Inverted-Y shaped structures and moving blobs can be identified in some events. A subset of these events also reveal signatures in the HRILyα (H i Lyα at 1216 Å) images and the extreme ultraviolet images taken by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). Our differential emission-measure (EM) analysis suggests a multithermal nature and an average density of ∼1.4 × 109 cm−3 for these microjets. Their thermal and kinetic energies were estimated to be ∼3.9 × 1024 erg and ∼2.9 × 1023 erg, respectively, which are of the same order of the released energy predicted by the nanoflare theory. Most events appear to be located at the edges of network lanes and magnetic flux concentrations, suggesting that these coronal microjets are likely generated by magnetic reconnection between small-scale magnetic loops and the adjacent network field.

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Language(s): eng - English
 Dates: 2021
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: ISI: 000692239600001
DOI: 10.3847/2041-8213/ac1f30
 Degree: -

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Title: Astrophysical Journal, Letters
  Other : ApJL
Source Genre: Journal
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Publ. Info: Bristol, UK : Institute of Physics Publishing (IOP)
Pages: - Volume / Issue: 918 (1) Sequence Number: L20 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_1