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Statistical investigation of decayless oscillations in small-scale coronal loops observed by Solar Orbiter/EUI

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dc.contributor.author Shrivastav, Arpit Kumar
dc.contributor.author Pant, Vaibhav
dc.contributor.author Berghmans, David
dc.contributor.author Zhukov, Andrei N
dc.contributor.author Doorsselaere, Tom Van
dc.contributor.author Petrova, Elena
dc.contributor.author Banerjee, D
dc.contributor.author Lim, Daye
dc.contributor.author Verbeeck, Cis
dc.date.accessioned 2024-06-21T08:48:32Z
dc.date.available 2024-06-21T08:48:32Z
dc.date.issued 2024-05
dc.identifier.citation Astronomy & Astrophysics, Vol. 685, A36 en_US
dc.identifier.issn 0004-6361
dc.identifier.uri http://hdl.handle.net/2248/8490
dc.description Open Access. en_US
dc.description Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
dc.description.abstract Decayless kink oscillations are omnipresent in the solar atmosphere, and they are a viable candidate for coronal heating. Although there have been extensive studies of decayless oscillations in coronal loops with lengths of a few hundred megameters, the properties of these oscillations in small-scale (∼10 mm) loops are yet to be explored. In this study, we present the properties of decayless oscillations in small loops embedded in the quiet corona and coronal holes. We use high-resolution observations from the Extreme Ultraviolet Imager on board Solar Orbiter with pixel scales of 210 km and a cadence of 5 s or better. We analysed 42 oscillations in coronal loops with loop lengths varying between 3 to 23 mm. The average displacement amplitude is found to be 134 km. The oscillations period has a range of 28 to 272 s, and the velocity amplitudes range from 2.1 to 16.4 km s−1. The variation in the loop length with the period does not indicate a significant correlation. The wave mode of these waves is uncertain, and standing waves are one possibility. Our results for the coronal seismology and energy flux estimates were obtained considering standing modes. The observed kink speeds are lower than those observed in active region coronal loops. We obtain an average magnetic field value of 2.1 G. We estimated the energy flux with a broad range of 0.6-313 W m−2. Moreover, we note that short-period decayless oscillations are not prevalent in the quiet Sun and coronal holes. Our study suggests that decayless oscillations in small-scale coronal loops are unlikely to provide enough energy to heat the quiet Sun and accelerate solar wind in coronal holes. en_US
dc.language.iso en en_US
dc.publisher EDP Sciences en_US
dc.relation.uri https://doi.org/10.1051/0004-6361/202346670
dc.rights © The Authors 2024
dc.subject Magnetohydrodynamics (MHD) en_US
dc.subject Sun: corona en_US
dc.subject Sun: oscillations en_US
dc.title Statistical investigation of decayless oscillations in small-scale coronal loops observed by Solar Orbiter/EUI en_US
dc.type Article en_US


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