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arxiv: 2606.04732 · v1 · pith:3LOYCCS7new · submitted 2026-06-03 · 🌌 astro-ph.SR

Recurrent Coronal Jets and QPPs: Periodic Reconnection and Localized Heating Across Quiet-Sun to Active Regions

Sudheer K. Mishra , Kartika Sangal , Balveer Singh , Ayumi Asai , A. K. Srivastava , Ding Yuan This is my paper

Pith reviewed 2026-06-28 04:27 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords coronal jetsquasi-periodic pulsationsmagnetic reconnectionfan-spine topologysolar corona heatingflux emergencequiet Sunactive regions
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The pith

Periodic reconnection in fan-spine topologies drives recurrent coronal jet eruptions and localized heating from quiet Sun to active regions.

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

The paper examines three long-lived recurring coronal jets observed with SDO/AIA across quiet Sun, moderate-field, and active regions. Wavelet analysis of EUV light curves at the jet bases reveals quasi-periodic pulsations with periods of 6-13 minutes. Distance-time maps show propagating ridges interpreted as repeated plasma ejections, while differential emission measure analysis finds multithermal plasma with peak temperatures near the base. Photospheric unsigned flux measurements at the sources exhibit periodicities of 10-32 minutes that align with the jet recurrence, favoring episodic reconnection over wave-driven explanations. The QPP periods fall well below radiative and conductive cooling times, pointing to ongoing localized energy input within the fan-spine magnetic setup.

Core claim

Periodic magnetic reconnection driven by successive flux emergence in fan-spine topologies produces recurrent jet eruptions accompanied by quasi-periodic pulsations of 6-13 min. The dominant photospheric flux periodicities of 10-32 min at the source regions support the reconnection interpretation. Multithermal plasma persists with hottest material at the jet base, and the observed periods are shorter than cooling timescales, implying continuous localized coronal heating across quiet-Sun to active-region environments.

What carries the argument

Fan-spine magnetic topologies that enable episodic reconnection tied to successive flux emergence.

If this is right

  • The same reconnection process operates across quiet Sun, moderate-field regions, and active regions to produce recurrent jets.
  • Localized coronal heating is maintained by repeated small-scale reconnection events rather than isolated large events.
  • QPP periods in multithermal EUV emission serve as a signature of ongoing flux-emergence-driven reconnection cycles.
  • Plasma at jet bases remains multithermal because heating episodes outpace radiative and conductive losses.

Where Pith is reading between the lines

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

  • This mechanism offers a pathway for estimating the contribution of small-scale reconnection to the overall quiet-Sun coronal energy budget.
  • Similar periodic flux signatures could be checked in other dynamic coronal features such as microflares or loop oscillations.
  • Higher-cadence vector magnetograms would allow direct tracking of flux-emergence episodes to test the timing link with each jet.

Load-bearing premise

Periodic changes in photospheric unsigned flux are taken as the direct driver of reconnection rather than a coincidental or secondary effect.

What would settle it

Recurrent jets exhibiting the same QPP periods but lacking corresponding 10-32 min periodicities in the underlying photospheric flux would undermine the reconnection-driven explanation.

Figures

Figures reproduced from arXiv: 2606.04732 by A. K. Srivastava, Ayumi Asai, Balveer Singh, Ding Yuan, Kartika Sangal, Sudheer K. Mishra.

Figure 1
Figure 1. Figure 1: Multi-wavelength observations of Jet 1 from the quiet-Sun region. (a) SDO/HMI LOS [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Same as Figure 1 but for Jet 2 from a moderate-field-strength region of the Sun. [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Same as Figure 1 but for Jet 3 from an evolving active region. Panels (a)-(h) correspond to the [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Wavelet analysis for jet1 extracted from the light curve from the base of the anemone jets. The top [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Similar to Figure 4 but for Jet2 [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Similar to Figure 4 but for Jet3 during its initial anemone jet phase (01:00 and 05:00 UT on June [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Similar to Figure 4 but for Jet3 during its eruptive phase (05:00-10:30 UT on June, 1 [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Top panel: Panels (a) and (b) depict the EM map and EM weighted-temperature map for Jet 1 at [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗
read the original abstract

We analyze quasi-periodic pulsations (QPPs) in recurrent coronal jets driven by periodic magnetic reconnection associated with successive flux emergence in the fan-spine magnetic topologies. Using the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO), we investigate three long-lived recurring jets spanning quiet Sun to moderate-field-strength regions, each exhibiting recurrent eruptions linked to episodic reconnection. Wavelet analysis of multithermal AIA EUV jet-base light curves detects QPPs with periods of 6-13 min, exceeding typical p-mode oscillation periods. Distance-time analysis reveals quasi-periodic propagating ridges, interpreted as recurrent field-aligned plasma ejections, and morphological similarities to slow magnetoacoustic waves, which cannot be entirely excluded. However, the dominant photospheric unsigned flux periodicities of 10-32 min at the jet source regions favor the reconnection-driven interpretation. DEM analysis confirms multithermal plasma with the hottest emission concentrated near the jet base, and the QPP periods fall well below both radiative and conductive cooling timescales, implying persistent localized heating within the fan-spine configuration. These results demonstrate that periodic reconnection in fan-spine topologies drives recurrent jet eruptions and contributes to localized coronal heating across the quiet Sun, moderate-field strength regions, and active regions.

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

1 major / 1 minor

Summary. The manuscript analyzes three long-lived recurrent coronal jets observed with SDO/AIA across quiet-Sun to active-region regimes. Wavelet analysis of multithermal EUV light curves at the jet bases detects QPPs with periods 6-13 min; distance-time maps show quasi-periodic propagating ridges; DEM confirms multithermal plasma with hottest emission near the base; and photospheric unsigned-flux time series exhibit dominant periods 10-32 min. The authors interpret the flux periodicities as favoring periodic reconnection in fan-spine topologies over wave mechanisms, with the QPPs falling below cooling timescales implying persistent localized heating.

Significance. If the reconnection interpretation is placed on a firmer quantitative footing, the comparative analysis across solar regimes would add useful observational constraints on how episodic flux emergence can drive recurrent jets and contribute to localized coronal heating. The application of standard tools (wavelet periodograms, DEM, distance-time analysis) is internally consistent and reproducible; the multithermal structure and period range below cooling times are solid supporting elements.

major comments (1)
  1. [Abstract] Abstract: the assertion that 'dominant photospheric unsigned flux periodicities of 10-32 min at the jet source regions favor the reconnection-driven interpretation' is not supported by a demonstrated causal or temporal linkage to the 6-13 min coronal QPPs. No timing correlation, phase analysis, or explicit test excluding upward-propagating slow-wave trains is described; the periods overlap only partially and the preference for reconnection therefore remains correlative rather than exclusionary.
minor comments (1)
  1. [Abstract] Abstract: the parenthetical remark that morphological similarities to slow magnetoacoustic waves 'cannot be entirely excluded' would benefit from a short quantitative note on expected wave periods or propagation speeds for the observed structures.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the constructive report and the recommendation for major revision. We address the single major comment below, agreeing that the abstract language requires clarification to avoid overstating the evidence.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the assertion that 'dominant photospheric unsigned flux periodicities of 10-32 min at the jet source regions favor the reconnection-driven interpretation' is not supported by a demonstrated causal or temporal linkage to the 6-13 min coronal QPPs. No timing correlation, phase analysis, or explicit test excluding upward-propagating slow-wave trains is described; the periods overlap only partially and the preference for reconnection therefore remains correlative rather than exclusionary.

    Authors: We agree that the manuscript does not present a direct timing correlation, phase analysis, or explicit test to exclude upward-propagating slow magnetoacoustic wave trains. The periods show only partial overlap (flux variations 10-32 min versus QPPs 6-13 min), and the preference for reconnection is based on the detection of significant photospheric flux periodicities within the fan-spine topology rather than a demonstrated causal link. The abstract already notes that wave contributions cannot be entirely excluded. We will revise the abstract to replace the phrase 'favor the reconnection-driven interpretation' with 'provide supporting evidence consistent with a reconnection-driven interpretation, although wave contributions cannot be fully excluded.' This revision will be implemented in the next version of the manuscript. revision: yes

Circularity Check

0 steps flagged

No circularity: claims rest on direct observational period comparisons without self-referential derivation

full rationale

The paper presents no mathematical derivation chain, fitted parameters, or equations that reduce to their own inputs. Central claims rely on wavelet analysis of observed QPP periods (6-13 min), photospheric flux periodicities (10-32 min), and DEM results compared against known p-mode ranges and cooling timescales. The interpretation favoring reconnection over waves is explicitly correlative and acknowledges morphological similarities to waves cannot be excluded; no self-citation load-bearing, ansatz smuggling, or renaming of known results occurs. This is self-contained observational analysis against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The abstract invokes standard solar-physics domain assumptions about magnetic topology and cooling timescales but introduces no new free parameters, invented entities, or ad-hoc axioms beyond those.

axioms (2)
  • domain assumption Fan-spine magnetic topologies are present at the observed jet sources
    Central to interpreting the recurrent eruptions as reconnection-driven.
  • domain assumption QPP periods falling well below radiative and conductive cooling timescales imply persistent localized heating
    Used to conclude ongoing energy input rather than a single impulsive event.

pith-pipeline@v0.9.1-grok · 5782 in / 1402 out tokens · 42622 ms · 2026-06-28T04:27:36.502842+00:00 · methodology

discussion (0)

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