Fast and periodic propagating disturbances along coronal loops detected with EUI on board Solar Orbiter
Abstract
Context. Recent high-resolution observations from the Solar Orbiter mission can help detect the indirect signatures of heating at the smallest scales. Aims. In this work, we measure the properties and investigate the physical origin of propagating disturbances (PDs) in the intensity at the smallest resolvable scales with Solar Orbiter/EUI along coronal loops. Methods. We used two sequences of EUI/HRIEUV at high spatial (down to 125 per pixel) and temporal resolutions (5 of cadence). We placed slits along 13 active region (AR) coronal loops. We measured the plane-of-sky (PoS) velocities and the intensity perturbation damping along the slits of PDs. We also measured the periodicity of PDs in one slit by using a Fourier analysis. Results. We report the detection of PDs that have high PoS velocities ranging between 500 and 2000 (which we call ``fast'' PDs). They are only visible in the upper part of the coronal loops. The intensity increase associated with these fast PDs is on the order of 4--8% of the HRIEUV intensity, and we measured little to no damping of their intensity with distance. We also measured a peak in the Fourier power spectra at 2 min above the 95% confidence limit that is associated with fast PDs. The fast PDs are detected in the same coronal loops as PDs with a lower PoS velocity (70--90), which we refer to as ``slow'' PDs. Unlike the fast PDs, these slow PDs are only visible in the lower part of the coronal loop, and they show clear intensity damping. Conclusions. Slow PDs show properties consistent with slow magneto-acoustic modes or upflows. On the other hand, fast PDs cannot be explained by slow magneto-acoustic modes. Instead, they show properties consistent with fast flows induced by magnetic reconnection, current sheet generated by propagating transverse oscillations, and fast magnetohydrodynamics modes or Alfvén waves.
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BibTeX
@article{dolliou2026fast,
title = {{Fast and periodic propagating disturbances along coronal loops detected with EUI on board Solar Orbiter}},
author = {A. Dolliou and S. Mandal and K. Barczynski and T. van Doorsselaere and D. Berghmans and C. Froment and F. Auchère and P. Antolin and H. Eklund and Y. Zhu and E. Kraaikamp and C. Verbeeck},
journal = {Astronomy \& Astrophysics - A\&A},
year = {2026},
month = oct,
doi = {10.1051/0004-6361/202660882},
eprint = {2607.17821},
archivePrefix = {arXiv},
url = {https://insu.hal.science/insu-05798986v1},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Fast and periodic propagating disturbances along coronal loops detected with EUI on board Solar Orbiter
AU - A. Dolliou
AU - S. Mandal
AU - K. Barczynski
AU - T. van Doorsselaere
AU - D. Berghmans
AU - C. Froment
AU - F. Auchère
AU - P. Antolin
AU - H. Eklund
AU - Y. Zhu
AU - E. Kraaikamp
AU - C. Verbeeck
PY - 2026
DA - 2026/10/14
JO - Astronomy & Astrophysics - A&A
DO - 10.1051/0004-6361/202660882
UR - https://insu.hal.science/insu-05798986v1
AB - Context. Recent high-resolution observations from the Solar Orbiter mission can help detect the indirect signatures of heating at the smallest scales. Aims. In this work, we measure the properties and investigate the physical origin of propagating disturbances (PDs) in the intensity at the smallest resolvable scales with Solar Orbiter/EUI along coronal loops. Methods. We used two sequences of EUI/HRIEUV at high spatial (down to 125 per pixel) and temporal resolutions (5 of cadence). We placed slits along 13 active region (AR) coronal loops. We measured the plane-of-sky (PoS) velocities and the intensity perturbation damping along the slits of PDs. We also measured the periodicity of PDs in one slit by using a Fourier analysis. Results. We report the detection of PDs that have high PoS velocities ranging between 500 and 2000 (which we call ``fast'' PDs). They are only visible in the upper part of the coronal loops. The intensity increase associated with these fast PDs is on the order of 4--8% of the HRIEUV intensity, and we measured little to no damping of their intensity with distance. We also measured a peak in the Fourier power spectra at 2 min above the 95% confidence limit that is associated with fast PDs. The fast PDs are detected in the same coronal loops as PDs with a lower PoS velocity (70--90), which we refer to as ``slow'' PDs. Unlike the fast PDs, these slow PDs are only visible in the lower part of the coronal loop, and they show clear intensity damping. Conclusions. Slow PDs show properties consistent with slow magneto-acoustic modes or upflows. On the other hand, fast PDs cannot be explained by slow magneto-acoustic modes. Instead, they show properties consistent with fast flows induced by magnetic reconnection, current sheet generated by propagating transverse oscillations, and fast magnetohydrodynamics modes or Alfvén waves.
SN - 0004-6361
SN - 1432-0746
ER -