Spatially resolved signatures of bi-directional flows observed in inverted-Y shaped jets

C. J. Nelson; M. Mathioudakis; N. Freij; R. Erd\'elyi; S. Bennett

REVIEW 3 major objections 4 minor 40 references

Spatially resolved signatures of bi-directional flows observed in inverted-Y shaped jets

T0 review · 3 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read Inverted-Y shaped jets near the solar limb show sustained red-to-blue H-alpha wing asymmetries along their legs, interpreted as bi-directional reconnection flows, and are followed minutes later by surges.

desk verdict A careful two-event SST/CRISP observation of inverted-Y jets with a red-to-blue wing asymmetry along the leg, but the bi-directional flow claim is weakened by an unaddressed line-of-sight projection degeneracy. read the letter →

arxiv 1908.05132 v1 pith:CLC2XRMJ submitted 2019-08-14 astro-ph.SR

C. J. Nelson , N. Freij , S. Bennett , R. Erdélyi , M. Mathioudakis This is my paper · ORCID

classification astro-ph.SR

keywords inverted-Yshapedjetsbi-directionalflowsmagneticreconnectionH-alphalineasymmetrieschromosphericsurgesslow-modeshockssolarphotosphereanemone

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 spatially resolved evidence that the legs of two inverted-Y shaped jets near the solar limb contain bi-directional plasma flows. In H-alpha line profiles, the authors find a sustained transition from red-shifted to blue-shifted asymmetries as one moves from the base to the top of each jet leg, lasting for the full 6-9 minute lifetimes of the events. Because the asymmetries persist for more than two minutes and extend beyond ±1 Å, the paper argues they cannot be explained by foreground absorption events such as rapid blue excursions. The same locations later host chromospheric surges, with a roughly three-minute delay that the authors interpret as the travel time of slow-mode shocks from a photospheric reconnection site to the transition region. If correct, the result connects small-scale photospheric reconnection directly to the launching of surges in the upper atmosphere.

What carries the argument

The central object is the H-alpha line-wing asymmetry measured along the legs of inverted-Y shaped jets: a red-to-blue gradient in intensity between wing positions of roughly ±0.8 Å and ±2 Å. These asymmetries are the observable signature that would be produced by bi-directional reconnection outflows, and their persistence is what separates them from foreground absorption. The paper uses these profiles, together with the temporal sequencing of jet and surge, to argue for a causal chain: reconnection below the canopy excites slow-mode waves; those waves shock at the transition region and lift cool material into a surge. Supporting comparisons include the size and footpoint separation of the jets against reported anemone jet statistics, the line-wing-only appearance, the absence of brightenings in the 1600 Å and 1700 Å channels, and the EUV absorption of the surges.

What would settle it

A direct test would be to observe an inverted-Y jet with simultaneous spectropolarimetry in two chromospheric lines formed at different heights: if the red-to-blue transition is a real Doppler flow, both lines should show consistent velocity reversals at the same pixels, whereas foreground absorption would produce different patterns. A single inverted-Y jet with the same sustained morphology but no subsequent surge after ten minutes, and no detectable magnetic flux cancellation at its footpoint, would also weaken the claimed causal chain.

Watch

Extended reading notes

Core claim

The central claim is that inverted-Y shaped jets observed in the wings of H-alpha are the products of magnetic reconnection in the lower solar atmosphere, and that the reconnection outflows are directly visible. Along one leg of each jet, normalised H-alpha line profiles change from red-wing-enhanced at the footpoint to blue-wing-enhanced toward the top, a spatial pattern expected if plasma is ejected both toward and away from the observer from a reconnection region within the leg. These one-wing enhancements reach 20-40% of the background and extend to ±2 Å, well beyond the spectral range of rapid blue excursions, and they remain present throughout the jets' lifetimes. The absence of H-alpha core brightening places the reconnection below the chromospheric canopy, while the subsequent appearance of surges at the same footpoints, delayed by about three minutes, is consistent with slow-mode wave pulses generated at the reconnection site and shocking at the transition region. The authors present this as evidence that photospheric reconnection can drive both the jets and the surges.

Load-bearing premise

The load-bearing premise is that the sustained red-versus-blue H-alpha wing enhancements trace Doppler-shifted plasma moving oppositely along each jet leg, rather than line-of-sight superposition of unrelated absorbing or emitting structures or opacity effects.

Editorial extensions

If this is right

Inverted-Y jets can be produced by reconnection below the chromospheric canopy, without any H-alpha core brightening.
Bi-directional flows inside jet legs are observable when line-scanned H-alpha data have sufficient spatial resolution, and they persist for minutes rather than being transient.
A delay of about three minutes between jet onset and surge formation is consistent with slow-mode wave propagation from the photosphere to the transition region.
Surges can form at sites of photospheric reconnection even when the surges show no bright tips and appear in EUV absorption.
Recurrent surges at a single site can be driven by a repeating reconnection process.

Reading between the lines

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

If the red-to-blue gradient is a real Doppler signature, co-temporal observations in Ca II 8542 or Mg II h&k should show the same opposing Doppler shifts at the same pixels; future high-resolution spectropolarimeters can test this directly.
The same mechanism predicts that a statistical survey of inverted-Y jets should find that jets with sustained one-wing asymmetries are significantly more likely to be followed by surges than symmetric-wing jets.
Event B's two successive surges hint that a single reconnection site can produce repeated slow-mode shocks; time-distance diagrams with faster cadence could test whether every surge episode follows a jet onset with the same delay.
Because the paper's two events are a small sample, a larger statistical study is needed to establish that photospheric reconnection is generally a driver of surges.

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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

The thing to know: this is a well-observed pair of inverted-Y jets at the limb, and the sustained H-alpha wing asymmetries are real. The paper does what no one has done cleanly before—resolves the jet legs spectroscopically and shows the red-to-blue transition lasting minutes, not seconds. The argument against foreground Rapid Blue Excursions is solid: the asymmetries live beyond ±1 Å and persist for 6–9 minutes, far longer than any RBE. The surge connection is suggestive and the three-minute lag is consistent with a slow-mode wave interpretation. The writing is honest, the data reduction is standard (MOMFBD/CRISP), and the sample-size limitation is acknowledged up front. Credit where due: this is a legitimate step beyond the imaging-only studies of Shibata et al. and the hints in Zeng et al. and Tian et al.

The soft spots are real, though. The stress-test concern lands: with four sampled points along one leg, a single unidirectional flow along a curved field line can produce exactly the same red→symmetric→blue pattern, purely from projection. The paper never addresses this. It simply asserts that the asymmetry implies two counter-streaming flows. For that claim to hold, the authors need to show the leg's geometry doesn't curve enough in the plane of the sky, or find a line-core Doppler signature, or present a model of the expected projection. As written, the central conclusion—that these jets are formed by reconnection with bi-directional outflows—rests on an assumption that is not justified. That is load-bearing, not a minor quibble.

Then there are the usual observational gaps: no error bars on the wing intensity differences, no quantitative significance testing, no multi-Gaussian decomposition, and—irritatingly for a 2019 paper—no reduced data or code release. The single-Gaussian Doppler maps that show no significant line-of-sight velocities are also left unexplained; they are not contradictory, but they deserve a sentence about why a 30% wing enhancement wouldn't shift the centroid.

Who is this for? Solar physicists working on small-scale reconnection signatures, specifically those interested in chromospheric jets and surges. It is worth a serious referee: the observation is novel and the interpretation is plausible, but it needs to be hardened. I would send it to peer review, with a request that the referee force the authors to confront the projection degeneracy and add quantitative error analysis. If they can rule out the curved single-flow explanation, this becomes a nice result. Right now, it is a good observation looking for a stronger argument.

Referee Report

3 major / 4 minor

Summary. The paper presents SST/CRISP H-alpha imaging spectroscopy of two inverted-Y shaped jets observed at the solar limb in AR 11506. The jets are visible in the H-alpha line wings but not in the line core. Along one leg of each jet, the authors measure line-profile asymmetries that transition from red-wing enhancement at the footpoint to blue-wing enhancement at the top, sustained for the lifetime of the events (roughly 6-9 minutes). They interpret this as spatially resolved bi-directional flows produced by magnetic reconnection in the lower solar atmosphere, and they further report that surges appear at the same footpoints a few minutes later, which they interpret as slow-mode shock waves lifting chromospheric material. The paper explicitly argues against an RBE (Rapid Blue Excursion) interpretation using the sustained lifetime and the spectral extent of the asymmetries.

Significance. If the central interpretation holds, the paper would provide one of the first spatially resolved spectroscopic signatures of bi-directional reconnection outflows in inverted-Y shaped jets, a rare observational counterpart to cartoon reconnection models. The data quality is high, the comparison to RBE alternatives is a genuine strength, and the association with subsequent surges is an interesting and testable finding. However, the main advance (bi-directional flows) rests on a single diagnostic whose geometric interpretation is not unique, and the quantitative support for the sustained asymmetries is not fully demonstrated. The small sample size is acknowledged by the authors; the more serious issue is the need to rule out projection and single-flow interpretations.

major comments (3)

[Section 3.1, Fig. 4] The red-to-blue transition in the H-alpha wing asymmetries along the jet leg is the sole evidence for bi-directional flows. At the limb, however, a single unidirectional flow along a curved magnetic field line would produce exactly the same sign reversal in line-of-sight (LOS) velocity as the leg bends toward or away from the observer. The manuscript does not constrain the three-dimensional orientation of the jet leg, nor does it quantify whether the spatial variation of the asymmetry across the four sampled points is consistent with a single projected flow. No two-component line-profile fitting or independent Doppler-velocity check is provided to distinguish a single curved flow from counter-streaming flows. Because the bi-directional flow inference is load-bearing for the paper's central claim, this geometric degeneracy must be addressed before the reconnection interpretation can be accepted.
[Section 3.1, Fig. 5] The sustained red-blue intensity differences are presented without error bars or any estimate of the noise level in the CRISP data. The claim that the asymmetries persist for the full lifetime of the jets depends on these differences being real at each time step, but the figure shows only the raw difference and a smoothed running difference. The authors should quantify the photon noise and residual seeing-induced intensity fluctuations (e.g., from the background or from symmetric profiles) and demonstrate that the measured differences are statistically significant throughout the event lifetimes.
[Section 3.2, Doppler analysis] The paper reports that single-Gaussian fitting to the H-alpha profiles found no significant line-of-sight velocities 'co-spatial to either event' in terms of rotation or inclination. If this analysis includes the jet footpoints where the large wing asymmetries are measured, it is unclear how a strong red-blue asymmetry can coexist with a negligible Doppler shift from a single Gaussian fit. If the fitting was restricted to the surges only, the text is ambiguous and should state explicitly which pixels were analyzed. The relationship between the asymmetric wing profiles and the Gaussian-fit velocities needs to be clarified, since this bears directly on the claimed flow magnitudes.

minor comments (4)

[Section 3.2] There are several typographical errors, including 'apparant' (should be 'apparent') and 'receeded' (should be 'receded').
[Fig. 4 caption] The caption states that spectral profiles are 'normalised against the background intensity' but does not define how the background intensity is measured; please specify the reference pixel or region used for normalization.
[Abstract and Section 3.1] The abstract says the asymmetries are present for 'over two minutes', while the text reports lifetimes of 9 minutes and 6 minutes for Events A and B. The abstract should be made consistent with the longer durations.
[Throughout] The manuscript uses both 'line-of-sight' and 'line of sight'; please standardize the hyphenation, and similarly ensure consistent notation for H-alpha throughout.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity found: the paper reports an observational interpretation with no fitted parameter renamed as a prediction and no load-bearing self-citation chain.

full rationale

The paper is an empirical analysis of two inverted-Y shaped jets using high-resolution H-alpha spectroscopy, and its central inference—that sustained red-to-blue line-wing asymmetries indicate bi-directional flows—is a direct observational interpretation rather than a derivation from a fitted model. The authors compare their data to published cartoon models (Shibata et al. 2007; Singh et al. 2011) and to simulations (Takasao et al. 2013), but these references are used qualitatively as consistency checks, not as inputs whose parameters are fitted to the data. No equation in the paper defines the detected quantity in terms of the claimed conclusion, and no fitted parameter is subsequently renamed as a prediction. Self-citations (Nelson et al. 2013, 2015, 2016, 2017) appear only as background context for EB behavior, thresholds, and prior UV-burst observations; they are not the load-bearing basis for the bi-directional-flow claim. The slow-wave speed estimate is an illustrative calculation using assumed height differences rather than a fitted result, and the authors explicitly note the limitations of their small sample size. Possible objections, such as the line-of-sight projection degeneracy for a curved jet leg, are physical correctness risks rather than circular reasoning. The manuscript therefore contains no self-definitional step, no fitted input called a prediction, and no imported uniqueness theorem; the paper is self-contained as an observational study.

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

No free parameters are fitted to data; the paper is observational. The main assumptions are standard solar-physics interpretive steps, all stated explicitly in the text. No new physical entities are proposed.

assumptions (4)

domain assumption H-alpha line core forms in the upper chromosphere, so absence of core brightening implies reconnection below the canopy.
Invoked in Sect. 3.1 to argue that the jets are low-atmosphere phenomena.
domain assumption Asymmetric line profiles in the wings are produced by Doppler shifts from bulk flows.
Used throughout Sect. 3.1 to interpret red-blue asymmetries as bi-directional flows.
domain assumption The observed inverted-Y morphology is a magnetic reconnection topology.
Taken from the cited literature (Shibata et al. 2007) and used as the interpretive framework.
domain assumption Representative heights of 1000-2000 km between the reconnection site and the transition region are reasonable for estimating wave propagation speeds.
Used in Sect. 3.2 to compute slow-mode wave speeds; not load-bearing for the main claim of bi-directional flows.

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Cite this review

Pith. "Pith review of Spatially resolved signatures of bi-directional flows observed in inverted-Y shaped jets." pith.science (2026). https://pith.science/paper/CLC2XRMJ

@misc{pith2026190805132,
  author       = {Pith},
  title        = {Pith review of: Spatially resolved signatures of bi-directional flows observed in inverted-Y shaped jets},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/CLC2XRMJ}},
  note         = {Machine review of arXiv:1908.05132}
}

read the original abstract

Numerous apparent signatures of magnetic reconnection have been reported in the solar photosphere, including inverted-Y shaped jets. The reconnection at these sites is expected to cause localised bi-directional flows and extended shock waves; however, these signatures are rarely observed as extremely high spatial-resolution data are required. Here, we use H-alpha imaging data sampled by the Swedish Solar Telescope's CRisp Imaging SpectroPolarimeter to investigate whether bi-directional flows can be detected within inverted-Y shaped jets near the solar limb. These jets are apparent in the H-alpha line wings, while no signature of either jet is observed in the H-alpha line core, implying reconnection took place below the chromospheric canopy. Asymmetries in the H-alpha line profiles along the legs of the jets indicate the presence of bi-directional flows, consistent with cartoon models of reconnection in chromospheric anemone jets. These asymmetries are present for over two minutes, longer than the lifetimes of Rapid Blue Excursions, and beyond \pm 1 \AA\ into the wings of the line indicating that flows within the inverted-Y shaped jets are responsible for the imbalance in the profiles, rather than motions in the foreground. Additionally, surges form following the occurrence of the inverted-Y shaped jets. This surge formation is consistent with models which suggest such events could be caused by the propagation of shock waves from reconnection sites in the photosphere to the upper atmosphere. Overall, our results provide evidence that magnetic reconnection in the photosphere can cause bi-directional flows within inverted-Y shaped jets and could be the driver of surges.

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Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.

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