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arxiv: 2606.17361 · v1 · pith:M4QBIJ4Mnew · submitted 2026-06-15 · 🌌 astro-ph.SR

Extreme Ultraviolet Microflashes at Plume Bases: A Candidate for Powering the Corona and Solar Wind?

Navdeep K. Panesar , Sanjiv K. Tiwari , Meng Jin , Ayla Weitz , Ronald L. Moore , V. Aparna , Alphonse Sterling This is my paper

Pith reviewed 2026-06-27 01:53 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords solar plumesmicroflashescoronal heatingsolar windmagnetic reconnectionEUV observationsp-mode oscillationsunipolar magnetic field
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The pith

Network microflashes at solar plume bases arise from unipolar reconnection bursts that may power the corona and solar wind.

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

The paper identifies frequent fine-scale bright bursts, termed network microflashes, in EUV images at the bases of solar plumes where the magnetic field is unipolar. Roughly 20 microflashes occur at once in a plume base, with a new one beginning every second, each releasing about 10^24 erg. The authors interpret these as brief reconnections between crossed legs of unipolar field lines, often set off by five-minute p-mode oscillations. If the interpretation holds, the microflashes supply a steady energy input that can heat the open corona and drive the solar wind. This positions unipolar reconnection bursts as a candidate mechanism sustaining the heliosphere from the magnetic network.

Core claim

The central claim is that network microflashes result from fine-scale bursts of reconnection of crossed legs of unipolar magnetic field, that the bursts are often triggered by 5-minute p-mode oscillations, and that the bursts are candidates for powering the open-field corona and solar wind. Approximately 20 microflashes are ongoing within a plume base, with a new microflash starting every second, each with energy in the nanoflare range of 10^24 erg. A 3D data-driven global MHD model shows open magnetic field with fast solar wind for the plumes, supporting the view that unipolar microflashes sustain the heliosphere via unipolar-network-field reconnection bursts.

What carries the argument

Network microflashes observed in 174A EUV images at plume bases in unipolar flux, interpreted as fine-scale reconnection bursts between crossed legs of unipolar magnetic field lines.

If this is right

  • The aggregate energy release from microflashes at plume bases can maintain the temperatures of the open corona.
  • Reconnection bursts in unipolar fields provide a mechanism for accelerating the fast solar wind.
  • Five-minute p-mode oscillations frequently trigger the reconnection events that release the energy.
  • Unipolar network reconnection sustains the heliosphere from the base of plumes.

Where Pith is reading between the lines

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

  • Similar microflashes could appear in other unipolar magnetic regions on the Sun beyond plumes.
  • High-cadence EUV observations could map the exact geometry of the crossed field legs during each burst.
  • The one-per-second rate implies a continuous, distributed energy input that models of solar wind acceleration must incorporate.
  • If confirmed, this mechanism would link photospheric oscillations directly to coronal heating in open-field regions.

Load-bearing premise

The observed microflash energies are sufficient in aggregate and transfer efficiently via reconnection to sustain coronal temperatures and solar wind speeds rather than dissipating locally or falling short overall.

What would settle it

A measurement showing that the total energy released by all microflashes across a plume base is less than the energy required to maintain observed coronal temperatures and solar wind speeds.

Figures

Figures reproduced from arXiv: 2606.17361 by Alphonse Sterling, Ayla Weitz, Meng Jin, Navdeep K. Panesar, Ronald L. Moore, Sanjiv K. Tiwari, V. Aparna.

Figure 1
Figure 1. Figure 1: Examples of network microflashes at a plume base. Panel (a) shows an HRIEUV 174 Å image of a solar plume and several microflashes. The dotted-dashed white box in (a) outlines the field of view (FOV) displayed in panels (c–l). Panel (b) shows an unsharp mask version of the same image. Panels (c–g) and (h–l) display HRIEUV 174 Å images and unsharp masked images, respectively, of network microflashes in the p… view at source ↗
Figure 2
Figure 2. Figure 2 [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Automated detection of network microflashes. The different colored circles in panel (a) mark different microflashes detected over the entire HRIEUV time span. The white dashed region is the FOV searched for microflashes. The background image is the HRIEUV image at13:40:00. Each microflash is indexed (1– ∼6000) by its time of appearance, with color indicating detection time from red (earliest) to pink (late… view at source ↗
Figure 4
Figure 4. Figure 4: Magnetic Setting and Flux-strength histogram of 50 random manually selected microflashes. (a) Locations of the peak-bright￾ness centroids of the 50 microflashes, marked by yellow “+” symbols, overlaid on the HMI plume-base flux map. (b) Histogram of HMI flux-strengths measured at the 50 microflash centroids shown in panel (a). (E. R. Priest et al. 1994). This value is about an order-of￾magnitude lower than… view at source ↗
Figure 5
Figure 5. Figure 5: Models for the open magnetic field and the microflashes in the observed coronal plume. Panels (a–c) show the MHD model 3D field from the region of the 29-March-2023 plume. The radial magnetic field is shown at r = 1.006 Rs with gray scale. Selected field lines from the plume region are shown. The color on the field lines shows the radial velocity of solar wind. Panel (a) shows a similar point of view as th… view at source ↗
Figure 6
Figure 6. Figure 6: The first example of network microflashes at a plume base observed by HRIEUV (from [PITH_FULL_IMAGE:figures/full_fig_p015_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Histograms of the plane-of-sky speed (a), length (b), and lifetime (c) for the 50 manually selected network microflashes. The red histogram in (b) is the width of the microflashes. The bin size is different for length (235 km) and width (100 km) histograms. The mean values of the speed, length, width, and lifetime are 27.5 ± 11.5 km s−1 , 675 ± 250 km, 450 ± 95 km, and 30 ± 15 seconds, respectively. microf… view at source ↗
Figure 8
Figure 8. Figure 8: Results from the wavelet analysis. Panel (a) shows an HRIEUV 174 Å image and the red box shows the region that was analyzed. Panel (b) shows the normalized wavelet power spectrum, inside the red box of (a), as function of time and period. The wavelet spectrum shows the power as a function of time and period, over the time of the HRIEUV observations. The black dashed curve depicts the cone of influence the … view at source ↗
Figure 9
Figure 9. Figure 9: An example of network microflashes at a plume-base observed by HRIEUV and SDO on 26-October-2023. Panel (a) shows HRIEUV 174 Å image of solar plumes and microflashes. Panel (b) shows the unsharp mask version of the same image. Panel (c) shows the same FOV in AIA 171 Å. Panel (d) shows the line-of-sight photospheric magnetic flux in the same FOV. In panel (c), HMI contours, of levels ±20 G, at 09:33:271 UT … view at source ↗
Figure 10
Figure 10. Figure 10: Network microflashes at the base of a plume. Panels (a–d) show 174 Å HRIEUV images of the plume base region in the FOV that is shown within the solid white box region of Figure 9a. Panels (e–g) show the unsharp mask images of the same. The green arrows point to a network microflash through most of its life. The red circles enclose other microflashes that are visible in these HRIEUV frames. Banerjee, D., G… view at source ↗
Figure 11
Figure 11. Figure 11: Network microflashes in network away from the plume base. Panels (a–d) show the 174 Å HRIEUV images in the FOV of the dotted-dashed white box region of Figure 9a. Panels (e–g) show the unsharp mask versions of those images. The green arrow points to a network microflash through most of its life. The red circles enclose other microflashes that are visible in these HRIEUV frames. Lionello, R., Linker, J. A.… view at source ↗
Figure 12
Figure 12. Figure 12: The MHD model 3D field from the plume region in the 2023 October 26 observations. The radial magnetic field is shown at r = 1.006 Rs with gray scale. Selected field lines are shown from the plume region. The color on the field lines shows the radial velocity of the solar wind. Panel (a) shows a similar point of view as the observation. Panels (b) and (c) show a different point of view. The field lines in … view at source ↗
read the original abstract

Solar plumes - outflows of bright coronal plasma - are a major component of the open-magnetic-field corona and solar wind, but their driving mechanism remains uncertain. Here we report on network microflashes, fine-scale bright bursts captured by Solar Orbiters Extreme Ultraviolet Imager in 174A images encompassing magnetic network at the base of plumes. Because they sit in evidently unipolar magnetic flux, they are evidently a new, previously unidentified, kind of network event. Approximately 20 microflashes are ongoing within a plume base, with a new microflash starting every second. The energy for an average microflash is 1024 erg, in the range of nanoflares. A 3D data-driven global MHD model yields open magnetic field with fast solar wind for the investigated plumes. From our findings, we suggest that network microflashes result from fine-scale bursts of reconnection of crossed legs of unipolar magnetic field, that the bursts are often triggered by 5-minute p-mode oscillations, and that the bursts are candidates for powering the open-field corona and solar wind. That is, unipolar microflashes such as ours are plausibly from unipolar-network-field reconnection bursts that sustain the heliosphere.

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

2 major / 1 minor

Summary. The manuscript reports the observational detection of 'network microflashes' — fine-scale EUV brightening events at the bases of solar plumes using Solar Orbiter EUI 174Å data. These events occur in unipolar magnetic regions, with ~20 ongoing per plume base at a rate of one new event per second, each releasing ~10^24 erg. A 3D data-driven MHD model is used to confirm open magnetic field lines and fast solar wind for the plumes. The authors interpret the microflashes as resulting from fine-scale reconnection of crossed legs of unipolar fields, often triggered by 5-minute p-mode oscillations, and propose them as candidates for powering the open-field corona and solar wind.

Significance. If the energy sufficiency and transfer efficiency can be established, the identification of these unipolar reconnection events would offer a new, observationally grounded candidate mechanism for the long-standing coronal heating and solar wind acceleration problems, potentially linking photospheric dynamics to heliospheric outflows.

major comments (2)
  1. [Abstract] Abstract: The central interpretive claim that network microflashes are 'candidates for powering the open-field corona and solar wind' is not supported by any explicit area-integrated power calculation comparing the reported aggregate input (~10^24 erg per event at ~1 s^{-1} rate) against observed coronal heating requirements (~10^5–10^6 erg cm^{-2} s^{-1}), nor by evidence that reconnection energy is deposited at coronal heights rather than dissipated locally.
  2. [Abstract] Abstract and MHD model description: The 3D data-driven global MHD model is reported to yield open magnetic field with fast solar wind, but the text provides no indication that microflash energy contributions or reconnection dynamics are incorporated into or validated by the model, leaving the powering link as an untested assertion.
minor comments (1)
  1. [Abstract] The final sentence of the abstract ('That is, unipolar microflashes such as ours are plausibly from unipolar-network-field reconnection bursts that sustain the heliosphere.') repeats the suggestion without adding new information; consider condensing for clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful and constructive review. The comments highlight important points about the strength of our interpretive claims. We respond to each major comment below and indicate revisions where appropriate.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central interpretive claim that network microflashes are 'candidates for powering the open-field corona and solar wind' is not supported by any explicit area-integrated power calculation comparing the reported aggregate input (~10^24 erg per event at ~1 s^{-1} rate) against observed coronal heating requirements (~10^5–10^6 erg cm^{-2} s^{-1}), nor by evidence that reconnection energy is deposited at coronal heights rather than dissipated locally.

    Authors: We agree that an explicit area-integrated power budget was not provided in the manuscript. The reported event energy (~10^24 erg) and occurrence rate (~1 s^{-1} with ~20 simultaneous events per plume base) allow an order-of-magnitude estimate once a typical plume-base area is adopted from the literature; we will add this calculation in the revised manuscript to compare directly with the canonical coronal heating flux. On energy deposition height, the 174 Å channel response requires plasma at ~1 MK, indicating that at least a fraction of the released energy reaches coronal temperatures rather than being fully dissipated in the lower atmosphere. A full radiative-MHD treatment of energy transport lies beyond the present observational study but is noted as future work. revision: yes

  2. Referee: [Abstract] Abstract and MHD model description: The 3D data-driven global MHD model is reported to yield open magnetic field with fast solar wind, but the text provides no indication that microflash energy contributions or reconnection dynamics are incorporated into or validated by the model, leaving the powering link as an untested assertion.

    Authors: The 3D data-driven MHD simulation is used only to establish that the large-scale magnetic topology of the observed plumes is open and consistent with fast-wind solutions; it is driven by photospheric magnetograms and does not resolve or inject the sub-arcsecond reconnection events. The microflashes are therefore presented as an observational candidate mechanism whose energy contribution is not yet folded into the global model. We will clarify this distinction in the revised text so that the model result is understood as providing necessary context (open fields) rather than a direct validation of the microflash powering hypothesis. revision: no

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper reports new EUV observations of microflashes at plume bases, estimates their energies from the data, and invokes an independent 3D data-driven MHD model to confirm open fields and fast wind. The central suggestion that the events are candidates for powering the corona and solar wind is an interpretive inference drawn from these external inputs rather than any equation or self-citation that reduces the claim to a fitted parameter or prior result defined by the target conclusion. No load-bearing step matches the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Based on abstract only; the work relies on standard solar-physics assumptions about magnetic reconnection and p-mode oscillations but introduces no explicit free parameters, new entities, or ad-hoc axioms in the provided text.

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