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arxiv: 1906.10353 · v1 · pith:4PMXT4C4new · submitted 2019-06-25 · 🌌 astro-ph.SR

On the relation between transition region network jets and coronal plumes

Youqian Qi , Zhenghua Huang , Lidong Xia , Bo Li , Hui Fu , Weixin Liu , Mingzhe Sun , Zhenyong Hou This is my paper

Pith reviewed 2026-05-25 16:33 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords coronal plumesnetwork jetstransition regionmagnetic convergencesolar coronaphotospheric magnetic fieldsIRIS observationsAIA imaging
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The pith

Regions with stronger magnetic convergence produce faster network jets and visible coronal plumes.

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

The paper compares four network lane regions observed with AIA 171Å images for plumes, IRIS 1330Å for jets, and HMI magnetograms for photospheric fields. Plumes appear clearly only in the two regions where magnetic features are more compact, while jets exist in all four but reach greater heights and speeds where the fields converge more strongly. The authors propose that this convergence enables faster shocks or more small-scale reconnections that power both the dynamic jets and the plumes. The work connects transition-region activity directly to coronal structures through differences in underlying magnetism. If correct, it indicates that jet and plume properties share a common dependence on photospheric field geometry.

Core claim

Network jets rooted in regions with stronger magnetic convergence are higher and faster than those in weaker-convergence regions, and coronal plumes are visible only in the stronger-convergence regions, even though jets occur everywhere; the stronger convergence is suggested to supply conditions for faster shocks and more small-scale magnetic reconnection events that power the more dynamic jets and the plumes.

What carries the argument

The side-by-side comparison of jet height, jet speed, plume visibility, and magnetic compactness across four labeled network regions R1–R4.

If this is right

  • Stronger convergence correlates with jets that reach greater heights and speeds.
  • Visible plumes appear only where convergence is strong enough to support the necessary energy release.
  • Small-scale reconnection or shock processes are implicated as the shared driver for both jets and plumes.
  • Network regions can be ranked by magnetic compactness to predict which will host plumes.
  • The relation holds across regions that are all dominated by positive polarity.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Plume formation may require the same reconnection or shock events that accelerate the jets, rather than arising independently.
  • Mapping convergence strength across larger areas could identify likely plume sites without direct coronal imaging.
  • The pattern may extend to other network phenomena such as spicules or bright points that also depend on field convergence.

Load-bearing premise

The absence of plumes in the two weaker-convergence regions is caused by the convergence difference itself rather than by viewing angle, evolutionary stage, or other unmeasured factors.

What would settle it

Finding visible coronal plumes in additional network regions that show similarly weak magnetic convergence, or finding no difference in jet heights and speeds when convergence strength is matched.

Figures

Figures reproduced from arXiv: 1906.10353 by Bo Li, Hui Fu, Lidong Xia, Mingzhe Sun, Weixin Liu, Youqian Qi, Zhenghua Huang, Zhenyong Hou.

Figure 1
Figure 1. Figure 1: The context images for regions studied in the present. (a) The AIA 171 ˚A image giving an overview of the coronal structures in and around the studied regions. The contours (white lines) outline the boundaries of the coronal holes determined in the AIA 193 ˚A image. The region enclosed by the rectangle (green lines) is zoomed-in in panels (b–e), where show HMI magnetic features (b), AIA 1600 ˚A image (c), … view at source ↗
Figure 2
Figure 2. Figure 2: The magnetic field lines in the regions derived from the potential field extrapola￾tions based on data taken on December 1 (a), December 2 (b), December 3 (c) and December 4 (d). The green and purple lines are representative of open field lines and the white ones are close field lines. The yellow rectangles indicate the studied region as shown in Figure 1b–e. SOLA: plume_solphy.tex; 26 June 2019; 0:39; p. … view at source ↗
Figure 3
Figure 3. Figure 3: The statistical histograms of the lifetimes (a), heights (b) and speeds (c) of the network jets identified and tracked in the regions of “R1&R2” (red lines) and “R3&R4” (black lines). SOLA: plume_solphy.tex; 26 June 2019; 0:39; p. 17 [PITH_FULL_IMAGE:figures/full_fig_p017_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The procedures of the automatic network jet identification and tracking algorithm. (a) A network region (“R1”) observed in IRIS SJ 1330 ˚A. The yellow line indicates the base of the network jets originated in this network. The slices (red lines denoted by “1–4”) are used to identified jet-like features (see the text for details). (b) The IRIS SJ 1330 ˚A radiation variations along the slices 1–4. The local … view at source ↗
read the original abstract

Both coronal plumes and network jets are rooted in network lanes. The relationship between the two, however, has yet to be addressed. For this purpose, we perform an observational analysis using images acquired with the Atmospheric Imaging Assembly (AIA) 171{\AA} passband to follow the evolution of coronal plumes, the observations taken by the Interface Region Imaging Spectrograph (IRIS) slit-jaw 1330{\AA} to study the network jets, and the line-of-sight magnetograms taken by the Helioseismic and Magnetic Imager (HMI) to overview the the photospheric magnetic features in the regions. Four regions in the network lanes are identified, and labeled ``R1--R4''. We find that coronal plumes are clearly seen only in ``R1''&''R2'' but not in ``R3''&``R4'', even though network jets abound in all these regions. Furthermore, while magnetic features in all these regions are dominated by positive polarity, they are more compact (suggesting stronger convergence) in ``R1''&``R2'' than that in ``R3''&``R4''. We develop an automated method to identify and track the network jets in the regions. We find that the network jets rooted in ``R1''&``R2'' are higher and faster than that in ``R3''&``R4'',indicating that network regions producing stronger coronal plumes also tend to produce more dynamic network jets. We suggest that the stronger convergence in ``R1''&``R2'' might provide a condition for faster shocks and/or more small-scale magnetic reconnection events that power more dynamic network jets and coronal plumes.

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 / 3 minor

Summary. The paper performs an observational analysis of four network-lane regions (R1–R4) using AIA 171 Å images for coronal plumes, IRIS 1330 Å slit-jaw images for network jets, and HMI line-of-sight magnetograms. Plumes are reported only in R1 and R2, which also exhibit more compact positive-polarity magnetic features; an automated jet-tracking algorithm is developed and applied, showing that jets in R1 and R2 reach greater heights and speeds than those in R3 and R4. The authors conclude that stronger magnetic convergence favors both more dynamic jets and visible plumes, possibly via enhanced shocks or small-scale reconnection.

Significance. If the reported correlation between magnetic compactness, jet kinematics, and plume visibility survives controls for selection effects, the work would supply a useful observational link between transition-region network jets and coronal plumes. The automated jet-identification and tracking procedure constitutes a concrete methodological contribution that could be adopted by others.

major comments (3)
  1. [region selection (R1–R4)] Region identification and comparison (abstract and § describing R1–R4): the four regions are chosen and contrasted on the basis of plume visibility, so that the subsequent finding of more compact fields and faster/higher jets in the plume-present regions cannot isolate convergence as the causal variable; differences in viewing angle, evolutionary stage, or total unsigned flux are not shown to be matched.
  2. [magnetic features comparison] Magnetic compactness assessment (results section on HMI magnetograms): compactness is characterized only qualitatively (“more compact”) from line-of-sight magnetograms; no quantitative metric (flux-weighted separation, horizontal-field divergence, or filling factor) is supplied, nor are the regions normalized by total unsigned flux or latitude.
  3. [interpretation of results] Causal interpretation (final paragraph of abstract and discussion): the suggestion that stronger convergence “might provide a condition for faster shocks and/or more small-scale magnetic reconnection events” is offered without direct observational diagnostics of either mechanism, resting entirely on the correlation whose confounders have not been excluded.
minor comments (3)
  1. [abstract] Abstract contains the repeated word “the the photospheric”.
  2. [methods] The automated jet-tracking method is presented as new; its validation against manual identification or synthetic data should be shown explicitly (e.g., in a dedicated methods subsection or appendix).
  3. [figures and results] Figure captions and text should state the exact time intervals and number of jets tracked in each region so that the height/speed statistics can be reproduced.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive comments, which help clarify the scope and limitations of our observational study. We address each major comment below, indicating revisions where appropriate. Our responses focus on strengthening the presentation of the reported correlations without overstating causality.

read point-by-point responses

  1. Referee: [region selection (R1–R4)] Region identification and comparison (abstract and § describing R1–R4): the four regions are chosen and contrasted on the basis of plume visibility, so that the subsequent finding of more compact fields and faster/higher jets in the plume-present regions cannot isolate convergence as the causal variable; differences in viewing angle, evolutionary stage, or total unsigned flux are not shown to be matched.

    Authors: We agree that the regions were identified based on the presence (R1, R2) or absence (R3, R4) of visible plumes in AIA 171 Å images, and that this selection precludes a controlled isolation of magnetic convergence as the sole causal factor. The manuscript reports an observational correlation rather than a causal demonstration. In revision we will (i) explicitly state the selection criterion in the methods section, (ii) add a table comparing total unsigned flux, average latitude, and approximate evolutionary stage for the four regions, and (iii) discuss possible viewing-angle effects. The core finding—that plume-visible regions also show more compact positive-polarity fields and more dynamic jets—remains unchanged. revision: yes

  2. Referee: [magnetic features comparison] Magnetic compactness assessment (results section on HMI magnetograms): compactness is characterized only qualitatively (“more compact”) from line-of-sight magnetograms; no quantitative metric (flux-weighted separation, horizontal-field divergence, or filling factor) is supplied, nor are the regions normalized by total unsigned flux or latitude.

    Authors: We acknowledge that the description of magnetic compactness is qualitative. In the revised manuscript we will introduce a quantitative metric: the flux-weighted mean separation between positive-polarity concentrations within each network lane, computed from HMI line-of-sight magnetograms after a consistent flux threshold. We will also report the total unsigned flux for each region and confirm that all four regions lie at comparable latitudes (within ~5°). These additions will be placed in a new subsection of the results. revision: yes

  3. Referee: [interpretation of results] Causal interpretation (final paragraph of abstract and discussion): the suggestion that stronger convergence “might provide a condition for faster shocks and/or more small-scale magnetic reconnection events” is offered without direct observational diagnostics of either mechanism, resting entirely on the correlation whose confounders have not been excluded.

    Authors: The language in the abstract and discussion is already hedged (“might provide a condition”). We agree that the paper contains no direct diagnostics of shocks or reconnection (e.g., spectroscopic line broadening or non-thermal velocities). In revision we will (i) move the mechanistic suggestion to the discussion only, (ii) explicitly label it as speculative and dependent on the observed correlations, and (iii) cross-reference the new discussion of potential confounders added in response to the first comment. No new observational diagnostics will be added, as they lie outside the scope of the present imaging study. revision: partial

Circularity Check

0 steps flagged

No circularity: purely observational comparison with no derivations or fitted predictions

full rationale

The paper performs an observational study using AIA, IRIS, and HMI data on four network regions. Regions are selected and compared based on direct plume visibility in images; jet properties are measured via a newly developed automated tracking method; magnetic compactness is described qualitatively from magnetograms. No equations, parameter fits, predictions, or self-citations appear in the provided text. The central suggestion is an interpretive hypothesis linking observed compactness to jet/plume dynamics, not a reduction of any result to its own inputs by construction. This is a standard observational analysis with no load-bearing circular steps.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the assumption that line-of-sight magnetograms faithfully indicate convergence strength and that the four selected regions differ only in that property; no free parameters or invented entities are introduced.

axioms (1)
  • domain assumption Line-of-sight magnetograms from HMI represent the dominant photospheric magnetic polarity and compactness in the selected network lanes.
    Invoked when comparing magnetic features across R1–R4 to explain plume presence.

pith-pipeline@v0.9.0 · 5863 in / 1130 out tokens · 24806 ms · 2026-05-25T16:33:06.237572+00:00 · methodology

discussion (0)

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Reference graph

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