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arxiv: 2605.03961 · v1 · submitted 2026-05-05 · 🌌 astro-ph.HE

Recognition: unknown

The jet-shaped pipe morphology in planetary nebulae and core-collapse supernova remnants

Noam Soker , Jessica Braudo (Technion , Israel)
Authors on Pith no claims yet

Pith reviewed 2026-05-07 13:51 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords planetary nebulaecore-collapse supernova remnantsjet morphologyjittering jetshydrodynamic simulationpipe structuresupernova explosion mechanism
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The pith

Jets shape the pipe morphology observed in some planetary nebulae and core-collapse supernova remnants.

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

The paper examines narrow, faint zones called pipes in images of planetary nebulae and core-collapse supernova remnants. By comparing these to hydrodynamical simulations of explosions driven by multiple pairs of jets, it proposes that jets create these structures. The authors show examples where opposite narrow lobes in nebulae might merge into a single pipe. This similarity leads them to conclude that jets also formed the pipes in the supernova remnants. Such findings support the idea that jittering jets are the main way core-collapse supernovae explode.

Core claim

We compare images of core-collapse supernova remnants and jet-shaped planetary nebulae that have a pipe morphology with a hydrodynamical simulation of a massive star explosion with three pairs of jets. From the qualitative similarity, we suggest that jets shaped the pipes in these objects. The simulation reproduces opposite narrow lobes that can later merge to form a pipe. This strengthens the case for the jittering jets explosion mechanism as the primary explosion mechanism of core-collapse supernovae.

What carries the argument

The jittering jets explosion mechanism (JJEM), in which multiple pairs of jets explode the star and shape the remnant morphology, as demonstrated by three-dimensional hydrodynamic simulations.

Load-bearing premise

The assumption that visual resemblance between the observed pipe structures and the simulated jet lobes is enough to identify the shaping mechanism, without quantitative metrics or ruling out other possibilities.

What would settle it

A core-collapse supernova remnant showing a pipe morphology that hydrodynamic simulations without jets can also produce, or one where the pipe cannot be matched by any jet configuration.

Figures

Figures reproduced from arXiv: 2605.03961 by Israel), Jessica Braudo (Technion, Noam Soker.

Figure 1
Figure 1. Figure 1: An image of the Cygnus Loop CCSNR in the visible band adapted from Raymond et al. (2023); the marks in white are from Shishkin et al. (2024), who identified the pipe and a point-symmetric morphology. Soker & Akashi (2025) argued that the cavity is a circum-jet ring. The pipe is the long, dark, north-south region; the white-dashed line covers a short portion of it. claim it was shaped by a pair of opposite … view at source ↗
Figure 2
Figure 2. Figure 2: Images of SNR G292.0+1.8. (a) An image from the Chandra site (Credit: X-ray: NASA/CXC/Penn State/Park et al. 2007; Optical: Pal.Obs. DSS): Red (0.580-710 and 0.880-950 keV), Orange (0.980-1.100 keV), Green (1.280-1.430 keV), Blue (1.810-2.050 and 2.400-2.620 keV); Optical (white). We added labeling for the two ears identified by Bear et al. (2017) as jet-shaped structures, as well as for the north and sout… view at source ↗
Figure 3
Figure 3. Figure 3: Emission-line maps of PN NGC 6720 adapted from Wesson et al. (2026b), who conducted and analyzed observations by the William Herschel Telescope on La Palma. Each map indicates the emitting species and the associated creation energy. The contours are of [Fe v] emission and represent the iron bar; collisional excitation of Fe4+ (54.8 eV ionization potential) produces this line. Images are on a linear surface… view at source ↗
Figure 5
Figure 5. Figure 5: An image of the multipolar PN NGC 2371 adapted from G´omez-Gonz´alez et al. (2020). We added the dashed red line to indicate the pipe. Red, green, and blue correspond to [N ii], Hα, and [O iii], respectively. M 1-41 view at source ↗
Figure 4
Figure 4. Figure 4: IR JWST images of NGC 6720 adapted from Wesson et al. (2026b) and based on Wesson et al. (2024). We added the marks of the filaments and pipe. (a) MIRI F1000W with contours of [Fe v] 4227 ˚A. (b) MIRI F560W, which emphasizes H2 emission. launch the three jet pairs into an initially spherically symmetric Wolf–Rayet (WR) stellar model of a collaps￾ing massive stellar core. The innermost region of the initial… view at source ↗
Figure 6
Figure 6. Figure 6: An IR Spitzer image of PN M 1-41 adapted from Zhang et al. (2012): blue, green and red correspond to 3.6 µm, 5.8 µm, and 8.0 µm, respectively. They drew the dashed lines to sketch the extended bipolar structures. We term them filaments and term the pipe. Each of the six jets carries the same mass and en￾ergy, mj = 1.6 × 1031 g and Ek,j = 2 × 1050 erg, respec￾tively, and is active for the same duration ∆tj(… view at source ↗
Figure 7
Figure 7. Figure 7: Planetary nebulae that show two jet-shaped lobes (or more) that we suggest might later evolve to one long pipe. (a) An HST image of the young PN Hen 3-401 (Credit: European Space Agency and Pedro Garcma-Lario at ESA ISO Data Center) (b) A composite image of PN Hen 2-320 adapted from Hsia et al. (2014): blue is Hα, green is Hα+[N ii], and red is [N ii]. We added the marks of filaments and the pipe. ergy, we… view at source ↗
Figure 9
Figure 9. Figure 9: Similar to view at source ↗
Figure 10
Figure 10. Figure 10: A velocity map in the same plane as the upper panel of view at source ↗
read the original abstract

We compare images of core-collapse supernova (CCSN) remnants (CCSNRs) and jet-shaped planetary nebulae (PNe) that have a narrow, faint zone extending from side to side, termed a pipe, with a hydrodynamical numerical simulation exploding a massive star with three pairs of jets in the framework of the jittering jets explosion mechanism (JJEM), and conclude that jets shaped the pipes in these CCSNRs and PNe. We present two jet-shaped PNe with a pipe and three PNe with two opposite narrow jet-shaped lobes, and argue that in some cases the two opposite narrow lobes might merge to form one long, faint zone extending from side to side of the PN, namely, a pipe. From the qualitative similarity of the pipe morphology of the two CCSNRs we analyze with the pipe of the PNe, we suggest that jets also shaped the pipe of these CCSNRs. We strengthen this conclusion with a three-dimensional hydrodynamic simulation that reproduces two opposite narrow lobes, similar to those observed in PNe with lobes. These lobes can merge later to form a pipe. This paper is another in a series that strengthen the case for the JJEM as the primary explosion mechanism of CCSNe by comparing CCSNR morphologies with those of jet-shaped PNe.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The manuscript claims that the 'pipe' morphology—a narrow, faint zone extending side-to-side—observed in two core-collapse supernova remnants (CCSNRs) and several planetary nebulae (PNe) is shaped by jets. It presents qualitative image comparisons of PNe with pipes or opposite narrow lobes (arguing the latter can merge into pipes) and supports the extension to CCSNRs with a single 3D hydrodynamic simulation of a massive-star explosion using three pairs of jets in the jittering jets explosion mechanism (JJEM), which produces opposite narrow lobes said to be capable of merging into a pipe. The work is positioned as further morphological evidence for JJEM as the primary CCSN explosion mechanism.

Significance. If the jet interpretation is confirmed, the result would strengthen morphological analogies between jet-shaped PNe and CCSNRs, offering indirect support for the jittering jets mechanism. The current evidence base is limited to visual resemblance and one unvaried simulation, so the significance remains provisional pending quantitative validation.

major comments (3)
  1. [Morphological comparison of PNe and CCSNRs] The central claim that jets shaped the pipes in the two CCSNRs rests on qualitative side-by-side image comparison alone; no quantitative shape descriptors (e.g., aspect ratio, surface-brightness profile along the faint zone, or moment analysis) are reported for either the observed pipes or the simulated lobes.
  2. [Hydrodynamic simulation section] The 3D hydrodynamical simulation reproduces two opposite narrow lobes but does not demonstrate their subsequent merging into a pipe, nor does it vary jet parameters (energy, opening angle, jittering timescale) to test uniqueness or robustness against the observed morphology.
  3. [Discussion and conclusions] Alternative non-jet channels for producing narrow faint zones (e.g., asymmetric ejecta, Rayleigh-Taylor fingers, or ISM interaction) are not modeled or statistically excluded, leaving the jet interpretation as one possible but untested explanation.
minor comments (2)
  1. [Abstract] The abstract and introduction would benefit from explicitly naming the two CCSNRs analyzed and stating the total number of PNe presented.
  2. [Figures] Figure captions should include scale bars, orientation, and wavelength/frequency information for all images to facilitate direct comparison.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. We address each major point below and have revised the manuscript accordingly to improve its rigor while preserving the core morphological argument.

read point-by-point responses

  1. Referee: [Morphological comparison of PNe and CCSNRs] The central claim that jets shaped the pipes in the two CCSNRs rests on qualitative side-by-side image comparison alone; no quantitative shape descriptors (e.g., aspect ratio, surface-brightness profile along the faint zone, or moment analysis) are reported for either the observed pipes or the simulated lobes.

    Authors: We agree that quantitative descriptors would add value. Although morphological studies in this field often rely on visual comparison due to projection effects and limited resolution, we have added aspect-ratio measurements for the pipes and lobes in both the observed objects and the simulation output. A short discussion of surface-brightness profiles along the faint zones has also been included where the data allow. revision: yes

  2. Referee: [Hydrodynamic simulation section] The 3D hydrodynamical simulation reproduces two opposite narrow lobes but does not demonstrate their subsequent merging into a pipe, nor does it vary jet parameters (energy, opening angle, jittering timescale) to test uniqueness or robustness against the observed morphology.

    Authors: The simulation was intended to show that the jittering-jets mechanism can produce the narrow, oppositely directed lobes seen in certain PNe; the text already states that these lobes are expected to merge into a pipe at later times. A full parameter survey is beyond the scope of the present work, but we have expanded the simulation section to reference earlier JJEM studies that explored variations in energy, opening angle, and jittering timescale, and we have clarified the evolutionary path to merging. revision: partial

  3. Referee: [Discussion and conclusions] Alternative non-jet channels for producing narrow faint zones (e.g., asymmetric ejecta, Rayleigh-Taylor fingers, or ISM interaction) are not modeled or statistically excluded, leaving the jet interpretation as one possible but untested explanation.

    Authors: We acknowledge that other mechanisms could in principle generate narrow faint zones. The revised discussion now explicitly lists these alternatives and explains why the close morphological match to jet-shaped PNe favors the jet interpretation in the present cases, while noting that a statistical exclusion of all alternatives would require modeling efforts outside the scope of this paper. revision: yes

Circularity Check

0 steps flagged

No significant circularity; morphological comparison and illustrative simulation are self-contained

full rationale

The paper advances its claim through side-by-side image comparison of observed pipe morphologies in two CCSNRs with those in PNe, plus one 3D hydrodynamical run that injects three jet pairs and produces narrow opposite lobes capable of later merging. This run is presented as a consistency check within the JJEM framework rather than a derivation in which any claimed result (e.g., the pipe shape) is mathematically identical to the input jet parameters by construction. No equations, fitted parameters renamed as predictions, or self-cited uniqueness theorems appear in the provided text that would force the conclusion from the assumptions. The reference to the authors' prior series supplies context for the framework but does not bear the logical load of the morphological analogy itself. The chain therefore rests on external observational images and a numerical illustration, remaining independent of its own inputs.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The paper takes the jittering jets explosion mechanism as the operative framework and interprets all morphologies inside it; no independent derivation of jet parameters or falsifiable predictions outside the model are provided.

free parameters (1)
  • jet parameters in the hydro simulation
    Three pairs of jets with specific directions and strengths are chosen to reproduce the observed lobes; these are adjusted to match the target morphology.
axioms (1)
  • domain assumption The jittering jets explosion mechanism is the primary explosion mechanism of core-collapse supernovae
    Invoked throughout the abstract as the context for the simulation and the interpretation of both planetary nebulae and supernova remnants.

pith-pipeline@v0.9.0 · 5534 in / 1290 out tokens · 39643 ms · 2026-05-07T13:51:29.090841+00:00 · methodology

discussion (0)

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Works this paper leans on

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