Extremely diverse coronal jets accompanying an erupting filament captured by Solar Orbiter

Alexander Warmuth; Fanpeng Shi; Fr\'ed\'eric Schuller; Jake A. J. Mitchell; Song Tan; Yuandeng Shen

REVIEW 3 major objections 4 minor 86 references

Extremely diverse coronal jets accompanying an erupting filament captured by Solar Orbiter

T0 review · 3 major / 4 minor · reviewed 2026-08-05 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Solar Orbiter's high-resolution EUV imager resolved nine coronal jets that lived only about 22 seconds each around an erupting limb filament on 2024 September 30, roughly 35 times shorter-lived than typical coronal jets, and attributes them

desk verdict A credible, well-observed discovery of extremely short-lived jets around a filament eruption, but the quantitative claims need error bars and a more careful census before the 'new class' label sticks. read the letter →

arxiv 2509.04741 v1 pith:7ZWRWPP6 submitted 2025-09-05 astro-ph.SR physics.space-ph

Song Tan , Alexander Warmuth , Frédéric Schuller , Yuandeng Shen , Jake A. J. Mitchell , Fanpeng Shi This is my paper · ORCID

classification astro-ph.SRphysics.space-ph

keywords coronaljetsfilamenteruptionmagneticreconnectionSolarOrbiterEUI/HRIEUVtransientextremeultravioletobservationslimb

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper reports the discovery of a previously unseen class of extremely short-lived coronal jets. Using Solar Orbiter's HRIEUV imager, which takes a 105-km-per-pixel image every two seconds, the authors watched a limb filament erupt and identified nine collimated plasma ejections with a median lifetime of 22 seconds — about 35 times shorter than the median lifetime found in large AIA-based surveys. The jets appeared in three phases of the eruption, becoming faster and shorter-lived as the eruption intensified. The paper argues they were driven not by the usual mini-filament mechanism but by dynamic magnetic reconnection between the rising large-scale filament and overlying magnetic fields, a mechanism that also explains why the jets are so transient.

What carries the argument

The central observational machinery is HRIEUV's unprecedented spatiotemporal resolution (105 km/pixel, 2 s cadence), combined with a frame-by-frame analysis recipe (Appendix C) that measures jet lifetimes by counting frames, widths by single-peak Gaussian fitting at 75% intensity-range edges, and velocities from displacement between a manually selected pair of frames. The physical mechanism proposed is magnetic reconnection between the erupting filament and overlying coronal fields, which naturally explains the short lifetimes (efficient energy conversion), the progressive velocity increase (intensifying reconnection), and the spatial separation of the rising-phase jets below the filament. T

What would settle it

Re-analyse the same HRIEUV dataset with a blind, automated jet-detection and tracking algorithm that does not require choosing frame pairs; if the detected features merge into continuous outflow or the recovered median lifetime exceeds about a minute, the central claim collapses. Alternatively, search for the predicted reconnection signatures — soft X-ray or radio bursts, plasmoid ejection — at the exact times and locations of jets 6–9 during 23:40–23:50 UT on 2024-09-30; their absence would contradict the reconnection mechanism.

Watch

Extended reading notes

Core claim

Using 1083 HRIEUV frames taken at 105 km/pixel and 2 s cadence during a 35-minute limb filament eruption on September 30, 2024, the authors identify nine transient coronal jets with a median lifetime of only 22 s and median speed of 385 km/s. The jets segregate into three groups by eruption phase: jets 1–3 during initiation show standard-jet morphology and slower speeds; jets 4–5 during the rising phase are bidirectional, originate below the filament, and are co-spatial with post-flare loop tops; jets 6–9 at peak show blowout-jet features with a three-pronged substructure. As the eruption progresses from initiation to peak, the jets become systematically shorter-lived and faster. The authors

Load-bearing premise

The whole measurement rests on the manual frame-by-frame identification of nine 'most prominent' jets and the properties taken from a few frames each — the authors themselves note the velocities 'may contain significant uncertainty depending on the selection of frames' — so if those selections are not reproducible, the 22-second median lifetime and the faster-toward-peak trend could be artefacts of how the frames were chosen.

Editorial extensions

If this is right

Previous AIA-based jet statistics missed an entire population of ultra-transient coronal jets; such 20-second-scale ejections are likely common around erupting filaments and have gone undetected due to temporal resolution limits.
Jet properties (lifetime, velocity, morphology) evolve systematically with eruption phase, so jets can serve as a real-time diagnostic of reconnection intensity during filament eruptions.
The proposed mechanism adds a new pathway for jet production — reconnection between a large-scale erupting filament and overlying fields — distinct from the established mini-filament trigger.
The shortest jets (e.g., jet 5, captured in only five frames) demonstrate that 2-second cadence is required to resolve this class, implying that future higher-cadence EUV observations will find many more such events.
The nine jets occurred after the first X-ray enhancement and follow the filament's rising height, tying their occurrence to the large-scale eruption dynamics rather than to random small-scale activity.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

If these jets are as widespread as the authors suspect, the energy and mass budget of filament eruptions includes a previously uncounted component of tiny, fast ejecta that may contribute to coronal heating and solar wind acceleration.
The phase-property trend (shorter lifetimes, higher velocities toward peak) makes a quantitative prediction: re-analyzing other HRIEUV flare-campaign events should reproduce a similar trend, and a failure to do so would indicate the trend is specific to this event's magnetic geometry.
The three-pronged substructure in jet 8, interpreted as filament threads in the reconnection outflow, could make such jets direct observational probes of a filament's internal magnetic structure if confirmed in additional events.
The downward-moving component of the rising-phase jets (jet 5) may be detectable in AIA 304 with appropriate time-shift corrections, providing an independent check on the 3D reconstruction and the proposed stretched-field reconnection.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Useful observational paper, and I largely agree with the reader's take. What is genuinely new is the dataset: nine very short-lived jets around a limb filament eruption on 2024-09-30, measured by Solar Orbiter HRIEUV at 2 s cadence. A median lifetime of 22 s is far below the typical AIA-derived median of ~13 minutes, and the phase-resolved grouping (initiation, rise, peak) is a nice organizational frame. The paper does solid scholarly work: it cites Chen et al. 2020 and Kumar et al. 2023, who reported similar transient jets around filaments, and it explicitly acknowledges three parallel studies on the same dataset. It also provides a detailed analysis recipe in Appendix C and makes the EUI data public. That is reproducible practice.

The soft spots are real but proportionate. The nine jets were selected as "most prominent" rather than by a complete census, so the sample is illustrative, not statistical. Velocities come from a single manually chosen frame pair per jet, and the authors admit these may carry significant uncertainty. Lifetimes are frame counts, so the 22 s median is inherently quantized to multiples of 2 s. The stress-test note is fair: no error bars, no sensitivity tests, and the phase trends (shorter lifetimes, higher velocities) rest on a manual recipe. A robustness test is needed.

That said, the central qualitative discovery survives. Even if individual lifetimes shift by a few seconds or a different frame pair changes a velocity by tens of percent, these jets are still dramatically shorter-lived than AIA-resolved jets. The qualitative claim does not depend on the exact median. The mechanism—reconnection between the erupting filament and overlying fields—is plausible and consistently argued, with a 3D reconstruction for the group 2 jets, and the authors explicitly concede that alternative mechanisms cannot be ruled out. That is honest.

Where the paper overreaches is in calling these jets a "previously unrecognised class." Given the prior work they cite, "distinct timescale and eruption context" is fairer than "new class." The overclaim is in the abstract and conclusions, and it should be toned down.

Bottom line: this deserves serious peer review. I would conditionally accept it with a request for error bars or at least a robustness appendix, a description of how the nine jets were selected, and a more measured classification. I would cite it in work on high-resolution EUV jets and would bring it to a reading group as a useful example of what HRIEUV reveals.

Referee Report

3 major / 4 minor

Summary. The paper presents Solar Orbiter EUI/HRIEUV observations of a limb filament eruption on 2024-09-30, identifying nine transient coronal jets in the 2-s-cadence 174 Å images. Using a frame-by-frame analysis, the authors report a median lifetime of ~22 s, median width ~330 km, and velocities of 85–540 km/s, and group the jets into three phases of the eruption. They propose that the jets are produced by reconnection between the erupting large-scale filament and overlying magnetic fields, with group 2 jets (below the filament) attributed to reconnection of stretched overlying fields. The paper includes a 3D reconstruction (HRIEUV + AIA) and appendices documenting the analysis.

Significance. These are among the shortest-lived coronal jets reported from EUV imaging, and if the measurements hold, they represent a genuinely new observational class enabled by HRIEUV's 2-s cadence. The paper is honest about projection effects and provides public data links, a detailed Appendix C, and per-jet image sequences (Figs. C.1–C.9), which allow independent verification. The main significance is empirical; the physical interpretation is plausible but not uniquely determined by single-wavelength data. The absence of quantified uncertainties is the main weakness.

major comments (3)

[Appendix C and §2.2] The central quantitative claims—22 s median lifetime, ~35× shorter than AIA jets, and the phase trend toward shorter/faster jets—rest entirely on the manual Appendix C recipe: lifetimes by counting 2 s frames, velocities from a single selected frame pair, edges at 75% of intensity range, widths from one Gaussian fit. Appendix C itself warns that velocities 'may contain significant uncertainty depending on the selection of frames,' yet no error bars or sensitivity tests appear in §2.2/Fig. 2. A one-frame difference changes lifetime by 2–4 s and can shift the median 22 s; another frame pair could reorder the 85–540 km/s sequence. This is load-bearing for the discovery claim. Please add explicit robustness tests (vary threshold, use all frames, multiple pairs) and report per-jet ranges.
[§2.1, §2.2, Fig. 2] The nine jets were chosen as 'the nine most prominent example jets' by subjective frame-by-frame examination. No operational selection criterion is given, and no census of all jet-like transients is presented. The phase trends (shorter lifetimes, higher velocities, group distinctions) could be an artifact of which jets were picked, especially with only 27 measurement points. Please state the selection rule quantitatively (e.g., minimum intensity contrast, morphological requirements) and test whether a different threshold or an unbiased automated detection reproduces the trends. At minimum, report how many other transient collimated features were present in the 60-min dataset and why they were excluded.
[Appendix B and §3.2] The proposed mechanism for group 2 jets—reconnection of overlying fields stretched by the filament—depends on the 3D reconstruction from a single AIA 171 wavelength pair and on co-spatiality with post-flare loops. The authors appropriately note in Appendix B that alternative mechanisms cannot be ruled out and that the side view limits the evidence; however, §4 conclusion 2 states this mechanism as a definitive result ('dynamic reconnection between the erupting filament and overlying magnetic fields produces these transient jets'). Please soften the conclusion to match the stated uncertainty, or add a quantitative test (e.g., derive the expected jet location from a potential-field model and compare with the reconstructed positions).

minor comments (4)

[Fig. A.2 caption] Typo: 'jet loction' should be 'jet location'.
[Throughout] Instrument name is written inconsistently as 'HRI EUV' and 'HRIEUV'; use one convention.
[§1] 'Spatial resolution of approximately 100 km/pixel' should be 'plate scale' or 'pixel scale,' since resolution is a derived quantity.
[Fig. 2 and Table (if any)] The heatmap in Fig. 2 would benefit from a companion table listing exact values with estimated uncertainties or ranges.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the measurements and inferred reconnection scenario do not reduce to their own inputs.

full rationale

The paper's central claims are observational: nine transient jets detected in HRIEUV images, with lifetimes/widths/velocities measured frame-by-frame (Appendix C), and a qualitative interpretation that reconnection between the erupting filament and overlying fields produced the jets. No equation is derived from the target result, no parameter is fitted to force a particular outcome, and no load-bearing step is justified by a self-citation chain. The Appendix C recipe (edges at 75% of the intensity range, Gaussian FWHM, manually chosen frame pairs, frame-counting lifetimes) is a measurement procedure, not a derivation that presupposes the conclusions; the paper explicitly flags the velocity uncertainty ('may contain significant uncertainty depending on the selection of frames') and the single-wavelength/interpretation limitation in Appendix B ('alternative mechanisms cannot be entirely ruled out'). These are legitimate robustness limitations, not circularity. The comparison with typical AIA jets uses an external large-sample benchmark (Musset et al. 2024) and independent reports of similar transient features (Kumar et al. 2023; Chen et al. 2020; Nóbrega-Siverio et al. 2025), so the short-lifetime claim is benchmarked externally rather than self-referentially. Self-citations (e.g., Tan et al. 2022, 2023; Duan et al. 2024) appear only in ordinary literature-review contexts about jet morphology and mini-filament triggers; they are not imported uniqueness theorems, ansätze, or fitting constraints. The reconnection mechanism is proposed as a consistent explanation of the observed spatial/temporal distribution and 3D reconstruction, not derived from itself. Thus no circular step is present; the honest finding is score 0.

Assumptions & free parameters 1 free parameters · 4 assumptions · 0 invented entities

The central claim rests on calibration of the instrument (provided by EUI level-2 data), the assumption that identified EUV features are real plasma ejections, and on manual analysis choices rather than fitted parameters. There are no invented entities; the mechanism is an interpretation of observed spatial/temporal coincidence.

free parameters (1)

Intensity edge threshold = 0.75 (three-quarters of the maximum-to-minimum range)
Appendix C: jet edges are defined where intensity drops to three-quarters of the range; this hand-chosen threshold directly sets measured widths and displacement-derived velocities.

assumptions (4)

domain assumption The bright moving features identified in HRIEUV long-exposure images are real coronal plasma structures, not image artifacts or jitter residuals.
Sec 2.2 and Appendix C: features as short as five frames (jet 5) are classified as jets; cross-correlation jitter reduction (Chitta et al. 2022) is applied but no artifact rejection is described.
domain assumption A single event observed from one EUV wavelength and one viewing geometry is representative enough to define a 'class' of phenomena.
Sec 2.1 and Conclusions: nine jets from one filament eruption are generalized into a previously unreported class with systematic phase trends; no multi-event control.
domain assumption STIX light-curve enhancements at 23:23 UT and 23:42 UT correspond to the claimed reconnection episodes (emerging flux loop interacting with filament, and main flare).
Sec 2.1 interprets STIX curves as reflecting initiation and main flare; attenuator intervention requires BKG detector substitution, adding uncertainty.
domain assumption Stereoscopic reconstruction using paired HRI and AIA 171 images (method of Nisticò 2023) gives reliable 3D positions for the filament, jets, and post-flare loops.
Appendix B: the group 2 mechanism relies on jets being co-spatial with post-flare-loop tops below the filament; the authors caution projection effects and single-wavelength limitation.

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Cite this review

Pith. "Pith review of Extremely diverse coronal jets accompanying an erupting filament captured by Solar Orbiter." pith.science (2026). https://pith.science/paper/7ZWRWPP6

@misc{pith2026250904741,
  author       = {Pith},
  title        = {Pith review of: Extremely diverse coronal jets accompanying an erupting filament captured by Solar Orbiter},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/7ZWRWPP6}},
  note         = {Machine review of arXiv:2509.04741}
}

read the original abstract

Solar jets are collimated plasma ejections driven by magnetic reconnection, which play a critical role in the energy release and mass transport in the solar atmosphere. Using Solar Orbiter's Extreme Ultraviolet Imager (EUI) with its unprecedented spatiotemporal resolution, we report the discovery of nine transient coronal jets associated with a filament eruption on September 30, 2024. These jets, with a median lifetime of only 22 seconds, have significantly shorter timescales than previously observed coronal jets. They exhibit diverse morphologies and properties, evolving through three distinct phases of the filament eruption: initiation, rise, and peak. The spatial and temporal distribution of the jets suggests they are driven by dynamic magnetic reconnection between the erupting filament and overlying magnetic fields. These jets represent a distinct class of phenomena different from traditional mini-filament-driven jets, being directly associated with large-scale filament eruption processes. This study reveals a previously unrecognised class of highly transient jets, highlighting the complexity of reconnection-driven processes during filament eruptions and underscoring the importance of high-resolution observations in uncovering fundamental plasma dynamics in the solar atmosphere.

Figures

Figures reproduced from arXiv: 2509.04741 by the authors.

**Figure 1.** (a) HRIEUV image (inverted colour scale) showing the erupting filament marked by a black rectangular box, with a length of approximately 80 Mm. (b) Magnified view of the erupting filament in HRIEUV, with gray rectangular boxes marking the locations of jets. (c) Most of the prominent frames of the nine jets, corresponding to the locations marked in (b). (d) STIX light curves in 4–10 keV and 25–50 keV bands (the backg… view at source ↗

**Figure 2.** Heatmap of properties for the nine jets, displaying lifetime, width, and velocity parameters with absolute values represented numerically while relative magnitudes are indicated by colour intensity. The normalised value here refers to each property divided by the maximum value of that property among the nine jets, represented through the colour map, offering a way to intuitively reflect the variation trend of each… view at source ↗

**Figure 3.** Group 1 jet representative: Jet 1 exhibiting standard jet morphology, with its key properties labeled (a1 and a2). The blue curve shows intensity distribution along the jet. Group 2 jet representative: Jet 4 displaying standard jet morphology with its key properties labeled (b1 and b2). Group 3 jet representative: Jet 8 showing blowout jet characteristics with its key properties labeled (c1 and c2). The blue curve… view at source ↗

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ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sent...
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write newline

" write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 gl...
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\@ifclassloaded agu2001 natbib The agu2001 class already includes natbib coding, so you should not add it explicitly Type <Return> for now, but then later remove the command natbib from the document \@ifclassloaded aguplus natbib The aguplus class already includes natbib codin...
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@stdbsttrue NAT@ctr \@lbibitem[ NAT@ctr ] \@lbibitem[#1]#2 \@extra@b@citeb \@ifundefined br@#2\@extra@b@citeb \@namedef br@#2 \@nameuse br@#2\@extra@b@citeb \@ifundefined b@#2\@extra@b@citeb @num @parse #2 [ @natanchorstart #2\@extra@b@citeb \@biblabel @num @natanchorend] @ifc...
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@open @close @open @close and [1] URL: #1 \@ifundefined chapter * \@mkboth \@ifundefined NAT@sectionbib * \@mkboth * \@mkboth\@gobbletwo \@ifclassloaded amsart * \@ifclassloaded amsbook * \@ifundefined bib@heading @heading NAT@ctr thebibliography [1] @ \@biblabel NAT@ctr \@bib...

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.

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