Analysis of a coronal hole jet in the chromosphere and the transition region with IRIS data and SDO observations
Abstract
Coronal jets are transient phenomena that occur throughout the solar atmosphere, often triggered by the activation of mini-filaments. Jets are an important field of study, as they are believed to contribute to the mass supply of the solar wind. We study a small-scale solar jet occurring in a low-latitude coronal hole, focusing on traces of the jet eruption to the lower atmosphere, utilizing chromospheric and transition region diagnostics. We also investigate the possible mechanisms and dynamic conditions leading to its onset. We analyze ultraviolet spectra from the Interface Region Imaging Spectrograph to investigate chromospheric dynamics and their connection to the transition region, using diagnostics of the Mg II k 2796.35 Å and Si IV 1393.75 Å lines, together with non-LTE inversions. We complement this analysis with multiwavelength imaging and magnetograms from the Solar Dynamics Observatory, as well as magnetic field modeling. The analysis of Mg II k and Si IV parameters reveals a coupling between chromospheric and transition region plasma dynamics. Profiles on the jet spire present deeper central reversals, larger peak separations and higher transition region Doppler velocities. The jet initiation is associated with a mini-filament-like structure, preceded by dynamic variations in the photospheric magnetic field. We find single-peaked Mg II k profiles at one of its footpoints, possibly indicating plasma drainage. The presence of a null point and a quasi-separatrix layer suggests that reconnection can play a role in the mini-filament-like structure destabilization and jet eruption. This study suggests that the signature and possibly the origin of coronal jets can be traced down to the chromosphere. The detailed analysis of the Mg II k profiles at the jet spire and the mini-filament-like structure may provide valuable observational constraints for future MHD simulations.
Related
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BibTeX
@misc{koletti2026analysis,
title = {{Analysis of a coronal hole jet in the chromosphere and the transition region with IRIS data and SDO observations}},
author = {M. Koletti and C. Gontikakis and S. Patsourakos and K. Tsinganos},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.31285},
eprint = {2610.31285},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.31285},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Analysis of a coronal hole jet in the chromosphere and the transition region with IRIS data and SDO observations
AU - M. Koletti
AU - C. Gontikakis
AU - S. Patsourakos
AU - K. Tsinganos
PY - 2026
DA - 2026/10/22
PB - arXiv
DO - 10.48550/arxiv.2610.31285
UR - https://arxiv.org/abs/2610.31285
AB - Coronal jets are transient phenomena that occur throughout the solar atmosphere, often triggered by the activation of mini-filaments. Jets are an important field of study, as they are believed to contribute to the mass supply of the solar wind. We study a small-scale solar jet occurring in a low-latitude coronal hole, focusing on traces of the jet eruption to the lower atmosphere, utilizing chromospheric and transition region diagnostics. We also investigate the possible mechanisms and dynamic conditions leading to its onset. We analyze ultraviolet spectra from the Interface Region Imaging Spectrograph to investigate chromospheric dynamics and their connection to the transition region, using diagnostics of the Mg II k 2796.35 Å and Si IV 1393.75 Å lines, together with non-LTE inversions. We complement this analysis with multiwavelength imaging and magnetograms from the Solar Dynamics Observatory, as well as magnetic field modeling. The analysis of Mg II k and Si IV parameters reveals a coupling between chromospheric and transition region plasma dynamics. Profiles on the jet spire present deeper central reversals, larger peak separations and higher transition region Doppler velocities. The jet initiation is associated with a mini-filament-like structure, preceded by dynamic variations in the photospheric magnetic field. We find single-peaked Mg II k profiles at one of its footpoints, possibly indicating plasma drainage. The presence of a null point and a quasi-separatrix layer suggests that reconnection can play a role in the mini-filament-like structure destabilization and jet eruption. This study suggests that the signature and possibly the origin of coronal jets can be traced down to the chromosphere. The detailed analysis of the Mg II k profiles at the jet spire and the mini-filament-like structure may provide valuable observational constraints for future MHD simulations.
ER -