Analysis of a coronal hole jet in the chromosphere and the transition region with IRIS data and SDO observations

arXiv:2610.31285 · astro-ph.SR · Submitted 2026-10-22 · Read on arXiv

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Introduction to the show: ident: Astrophysics Radio. Generated commentary on the latest astrophysics papers.

Vera: We're looking at the paper: "Analysis of a coronal hole jet in the chromosphere and the transition region with IRIS data and SDO observations".

Jocelyn: Here's the gist of the paper. The gist The study presents a comprehensive analysis of a small-scale solar jet occurring in a low-latitude coronal hole, focusing on traces of the jet eruption to the lower atmosphere using chromospheric and transition region diagnostics.

Jocelyn: The researchers analyzed ultraviolet spectra from the Interface Region Imaging Spectrograph (IRIS) 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 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 How it works The study utilized multiple observational data types to probe different atmospheric layers, including ultraviolet spectra from IRIS, multiwavelength imaging and magnetograms from the Solar Dynamics Observatory (SDO), as well as magnetic field modeling For chromospheric diagnostics, the optically thick Mg ii k line was used, while the Si iv 1393.75 Å and 1402.770 Å doublet lines were key emission lines for studying the dynamics of the solar transition region The analysis employed a genetic algorithm (GA) and Reinforcement Learning (RL) algorithms to fit spectral profiles, which significantly improved the fitting performance against noise and spectral profile variability How it works The results revealed a coupling between chromospheric and transition region plasma dynamics, evidenced by deeper central reversals, larger peak separations, and higher transition region Doppler velocities on the jet spire The jet initiation was linked to a mini-filament-like structure preceded by dynamic variations in the photospheric magnetic field Magnetic reconnection is believed to be the fundamental driver of solar jets, and spectroscopic evidence of this can manifest as bi-directional flows, such as downflows at the Mg ii k line and upflows at the Si iv line Magnetic reconnection can occur at null points or within quasi-separatrix layers (QSLs), which are suggested to be relevant in the mini-filament-like structure destabilization and jet eruption How it works The analysis of the magnetic topology using potential magnetic field extrapolation revealed closed magnetic field lines spatially coincident with the loop and open lines aligned with the jet spire The study found a null point at a height of 2 Mm above a photospheric parasitic (positive) polarity, also close to where the northern edge of the mini-filament-like structure is located 2.5 minutes later High Q values, log10Q≫2, indicate the presence of QSLs, where reconnection is likely to occur How it works The analysis of Mg ii k physical parameters showed statistically significant differences across regions, confirming that the jet and the background are distinct in several measured parameters The peak separation is correlated with the core depth and the k3 intensity for both structures, highlighting their distinction Furthermore, the jet exhibits strong dynamical effects detectable in both Mg ii and Si iv, while the loop doesn’t influence the chromosphere in such extent How it works The study concludes that the origin of the jet can be traced down to the chromosphere, as it is associated with a mini-filament whose formation is preceded by magnetic flux emergence, shear motions, and weak flux cancellation in the photosphere The appearance of the cooler jet component earlier than the hotter one, along with the location of the null point and the chromospheric response of all structures associated with the jet eruption, leads to this conclusion The novelty of this work is the use of GA and RL for the fitting of Mg ii and Si iv profiles, making the fits more robust against noise and spectral profile variability The size of the structures under study is close to the resolution limit of the related instruments, making the analysis of this kind challenging The paper provides insight into the genesis of a solar jet and its connection to chromospheric and transition region dynamics by combining IRIS and SDO observations.

Vera: The gist This study presents a comprehensive analysis of a small-scale solar jet occurring in a low-latitude coronal hole, focusing on traces of the jet eruption to the lower atmosphere using chromospheric and transition region diagnostics.

Paper summary: Vera: To recap, this paper's main goal is to study a small-scale solar jet in a low-latitude coronal hole by focusing on the eruption's traces down into the lower atmosphere using chromospheric and transition region diagnostics. They are also trying to figure out the possible mechanisms and dynamic conditions that lead to its onset.

Jocelyn: The core of their method involved using UV spectra from IRIS, specifically Mg ii k two thousand seven hundred ninety-six point three five Å and Si iv one thousand three hundred ninety-three point seven five Å, with non-LTE inversions to see the connection between the chromosphere and the transition region plasma dynamics.

Subrahmanyan: They also used multiwavelength imaging from SDO, magnetograms, and magnetic field modeling to look at the broader magnetic topology surrounding this jet event.

Vera: The results show that Mg ii k and Si iv parameters are coupled, meaning what's happening in the chromosphere is directly linked to what's happening in the transition region plasma.

Jocelyn: On the jet spire, they observed deeper central reversals, larger peak separations, and higher transition region Doppler velocities when looking at those specific spectral lines.

Subrahmanyan: The initiation of this jet was shown to be associated with a mini-filament-like structure that itself was preceded by dynamic variations in the photospheric magnetic field.

Vera: They also found single-peaked Mg ii k profiles at one of the footpoints, which they interpret as possibly indicating plasma drainage occurring at that location.

Jocelyn: The presence of a null point and a quasi-separatrix layer suggests that magnetic reconnection might be involved in destabilizing the mini-filament structure and driving the jet eruption.

Subrahmanyan: This paper connects the localized dynamics seen in the spectra to the larger context of magnetic field topology, showing how reconnection at null points or quasi-separatrix layers could be relevant here.

Conclusion: Vera: So looking at this work, "Analysis of a coronal hole jet in the chromosphere and the transition region with IRIS data and SDO observations," it really shows that we can probe these jets all the way down to where they start, right in the chromosphere.

Jocelyn: The authors connect what they see spectroscopically—those Mg ii k profiles—with their broader magnetic field observations from SDO, which is a big step for linking different atmospheric layers.

Subrahmanyan: What this suggests for us is that understanding the very first steps of a solar jet might hinge on seeing those fine structures in the chromosphere before they become visible higher up in the corona.

Vera: It gives us a new way to constrain future magnetohydrodynamic simulations by providing detailed observational data on how those jets are initiated and how they evolve right at their source.

Jocelyn: This work really highlights that solar jets aren't just things we see high up; the physics driving them is deeply embedded in the lower atmosphere.

Subrahmanyan: The next step for this kind of research would be to use these detailed Mg ii k profiles to test how different reconnection scenarios, like those involving null points, actually change the overall jet structure.

M. Koletti, C. Gontikakis, S. Patsourakos, K. Tsinganos

Department of Physics, National and Kapodistrian University of Athens · Research Center for Astronomy and Applied Mathematics, Academy of Athens · Physics Department, University of Ioannina

astro-ph.SR

Submitted: 2026-10-22

Updated: 2026-10-22

Comments: accepted for publication in Astronomy & Astrophysics

Code: https://github.com/FedericaChiti/Null_Finder

License: http://creativecommons.org/licenses/by/4.0/

Importance score: 63/100

The gist: The gist The study presents a comprehensive analysis of a small-scale solar jet occurring in a low-latitude coronal hole, focusing on traces of the jet eruption to the lower atmosphere using

Key concepts

Coronal Jets
These are transient phenomena in the solar atmosphere that occur when mini-filaments activate. They are important because they are thought to supply mass to the solar wind, and this study investigates their origin.
Chromospheric Diagnostics (Mg II k and Si IV)
The researchers used specific ultraviolet spectral lines, like Mg II k 2796.35 Å and Si IV 1393.75 Å, to probe the dynamics of the chromosphere. These diagnostics revealed a strong coupling between the chromospheric plasma behavior and the dynamics observed in the overlying transition region.
Mini-filament Structure
The jet's initiation is associated with a mini-filament-like structure in magnetic topology. This structure was preceded by dynamic changes in the photospheric magnetic field, indicating that localized magnetic instabilities are likely the trigger for jet eruption.

Summary

The gist The study presents a comprehensive analysis of a small-scale solar jet occurring in a low-latitude coronal hole, focusing on traces of the jet eruption to the lower atmosphere using chromospheric and transition region diagnostics.

How it works

  1. The researchers analyzed ultraviolet spectra from the Interface Region Imaging Spectrograph (IRIS) 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 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

How it works

The study utilized multiple observational data types to probe different atmospheric layers, including ultraviolet spectra from IRIS, multiwavelength imaging and magnetograms from the Solar Dynamics Observatory (SDO), as well as magnetic field modeling For chromospheric diagnostics, the optically thick Mg ii k line was used, while the Si iv 1393.75 Å and 1402.770 Å doublet lines were key emission lines for studying the dynamics of the solar transition region The analysis employed a genetic algorithm (GA) and Reinforcement Learning (RL) algorithms to fit spectral profiles, which significantly improved the fitting performance against noise and spectral profile variability

How it works

The results revealed a coupling between chromospheric and transition region plasma dynamics, evidenced by deeper central reversals, larger peak separations, and higher transition region Doppler velocities on the jet spire The jet initiation was linked to a mini-filament-like structure preceded by dynamic variations in the photospheric magnetic field Magnetic reconnection is believed to be the fundamental driver of solar jets, and spectroscopic evidence of this can manifest as bi-directional flows, such as downflows at the Mg ii k line and upflows at the Si iv line Magnetic reconnection can occur at null points or within quasi-separatrix layers (QSLs), which are suggested to be relevant in the mini-filament-like structure destabilization and jet eruption

How it works

The analysis of the magnetic topology using potential magnetic field extrapolation revealed closed magnetic field lines spatially coincident with the loop and open lines aligned with the jet spire The study found a null point at a height of 2 Mm above a photospheric parasitic (positive) polarity, also close to where the northern edge of the mini-filament-like structure is located 2.5 minutes later High Q values, log10Q≫2, indicate the presence of QSLs, where reconnection is likely to occur

How it works

The analysis of Mg ii k physical parameters showed statistically significant differences across regions, confirming that the jet and the background are distinct in several measured parameters The peak separation is correlated with the core depth and the k3 intensity for both structures, highlighting their distinction Furthermore, the jet exhibits strong dynamical effects detectable in both Mg ii and Si iv, while the loop doesn’t influence the chromosphere in such extent

How it works

The study concludes that the origin of the jet can be traced down to the chromosphere, as it is associated with a mini-filament whose formation is preceded by magnetic flux emergence, shear motions, and weak flux cancellation in the photosphere The appearance of the cooler jet component earlier than the hotter one, along with the location of the null point and the chromospheric response of all structures associated with the jet eruption, leads to this conclusion The novelty of this work is the use of GA and RL for the fitting of Mg ii and Si iv profiles, making the fits more robust against noise and spectral profile variability The size of the structures under study is close to the resolution limit of the related instruments, making the analysis of this kind challenging

The paper provides insight into the genesis of a solar jet and its connection to chromospheric and transition region dynamics by combining IRIS and SDO observations.

The gist

This study presents a comprehensive analysis of a small-scale solar jet occurring in a low-latitude coronal hole, focusing on traces of the jet eruption to the lower atmosphere using chromospheric and transition region diagnostics.

How it works

  1. The researchers analyzed ultraviolet spectra from the Interface Region Imaging Spectrograph (IRIS) 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

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

How it works

The study utilized multiple observational data types to probe different atmospheric layers, including ultraviolet spectra from IRIS, multiwavelength imaging and magnetograms from the Solar Dynamics Observatory (SDO), as well as magnetic field modeling

For chromospheric diagnostics, the optically thick Mg ii k line was used, while the Si iv 1393.75 Å and 1402.

Improvements for AI systems

  1. AI system can perform multi-layer solar atmosphere diagnostics by integrating highresolution chromospheric Mg ii k line analysis with transition region Si iv 1393 Å Doppler velocities to achieve a comprehensive understanding of jet initiation and evolution.

  2. The improved system can accurately predict the magnetic topology and reconnection likelihood by applying potential field extrapolation to SDO magnetograms, specifically identifying null points and quasi-separatrix layers where reconnection is likely to occur, based on the analysis of Figure 5.

  3. The AI can enhance spectral profile fitting robustness by implementing Reinforcement Learning (RL) algorithms to optimize seven-Gaussian fits for Mg ii k lines, improving the coefficient of determination R2 from 6% and 47% to 8% and 58% respectively.

  4. The system can statistically differentiate between jet and loop regions in solar plasma dynamics by calculating Spearman rank correlation coefficients between Mg ii k parameters (peak separation, core depth, RB asymmetry) and Si iv Doppler velocities (core and tail components).

  5. The improved AI can map the physical conditions of the jet spire by utilizing IRIS2 inversions to derive temperature, velocity, density, and microturbulence as a function of optical depth log tau for specific layers like log tau -4.8 or -5.6.

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.

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