pith. sign in

arxiv: 2605.17195 · v1 · pith:UHQVQ4KZnew · submitted 2026-05-16 · 🌌 astro-ph.SR

On the Nature of Candle-Flame-Shaped Solar Flares and Sub-Alfv\'enic Supra-Arcade Plasma Downflows

Ivan Oparin , Sabastian Fernandes , Bin Chen , Chengcai Shen , Xiaocan Li , Fan Guo , Sijie Yu This is my paper

Pith reviewed 2026-05-20 13:48 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords solar flaresmagnetic reconnectionsupra-arcade downflowscandle-flame morphologyMHD modelingY-pointsAlfvén speedprojection effects
0
0 comments X

The pith

In candle-flame solar flares the sites of magnetic reconnection do not coincide with the visible cusp tip and observed downflow speeds underestimate true Alfvén speeds by a factor of two to ten.

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

The paper uses three-dimensional magnetohydrodynamics simulations to study the magnetic geometry and plasma flows in flares that show a distinctive candle-flame or cusp shape in high-temperature EUV and X-ray images. It demonstrates that the Y-points, where the magnetic topology changes from antiparallel to closed field lines, can sit away from the apparent cusp tip seen in observations. The work also shows that tracks of downward plasma flows in time-distance plots yield speeds that are only lower limits on the actual Alfvén speeds in the reconnection inflow region. Projection effects and line-of-sight integration in the images are responsible for the apparent mismatch between observed and theoretical speeds.

Core claim

With the help of a recently developed three-dimensional magnetohydrodynamics model, the authors examine the locations where magnetic topology changes from antiparallel to closed (Y-points) in a candle-flame-shaped flare, compare the observational emission features with synthetic EUV images generated from the model, and analyze their time evolutions. They also investigate the role of projection effects and line-of-sight integration in the measurements of plasma downflow speeds. The analysis reveals that the Y-points do not necessarily coincide with the apparent cusp tip. The apparent speeds of the supra-arcade downflows, as derived from tracks in the time-distance plots, underestimate thetrue

What carries the argument

Three-dimensional magnetohydrodynamics model that produces synthetic EUV images and tracks magnetic topology changes to separate true Y-point locations from apparent cusp features while accounting for line-of-sight integration on downflow measurements.

If this is right

  • The brightest cusp seen in EUV or X-ray images does not always mark the exact site of ongoing reconnection.
  • Measured supra-arcade downflow speeds are lower bounds rather than direct measures of reconnection outflow speeds.
  • Synthetic forward modeling is required to correct for projection and line-of-sight effects when interpreting flare plasma flows.
  • Reconnection rate estimates based on observed downflow speeds alone will be too low.

Where Pith is reading between the lines

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

  • Reconnection theories may need to incorporate explicit three-dimensional field geometries when predicting observable flare morphology.
  • Energy-release calculations that rely on apparent flow speeds could be revised upward once projection corrections are applied.
  • Similar hidden offsets between apparent and true reconnection sites may occur in other astrophysical reconnection events such as in magnetospheres or accretion disks.

Load-bearing premise

The three-dimensional MHD model accurately reproduces the magnetic topology changes, emission features, and line-of-sight integration effects present in observed candle-flame-shaped solar flares.

What would settle it

High-resolution, multi-viewpoint EUV observations that locate the actual Y-point by tracing field-line connectivity and compare it directly to the position of the brightest cusp tip, or independent measurements of inflow Alfvén speeds that either match or exceed the apparent downflow speeds by the predicted factor.

Figures

Figures reproduced from arXiv: 2605.17195 by Bin Chen, Chengcai Shen, Fan Guo, Ivan Oparin, Sabastian Fernandes, Sijie Yu, Xiaocan Li.

Figure 1
Figure 1. Figure 1: Magnetic field geometry during the gradual phase of the solar flare, as derived from the numerical model (Shen et al. 2022). Black lines indicate a streamline plot of the magnetic field for the X-Y slice at coordinate z = 0. Background color map represents the magnitude of the magnetic field at timestep t = 3.0t0. The black dashed circle represents the above-the-looptop region where a topo￾logical transiti… view at source ↗
Figure 2
Figure 2. Figure 2: Reconnection current sheet geometry and magnetic field configuration at a selected time, t = 5.5t0, during the MHD model evolution. Central panel (b) shows the two-dimensional distribution of current density jz calculated for the single x–y slice of the simulation dataset. Overlaid in light gray are the streamlines of the magnetic field derived in the cutting plane. Blue and black markers show the bifurcat… view at source ↗
Figure 3
Figure 3. Figure 3: Observed and modeled EUV images of the candle-flame-shaped flare that occurred on July 19, 2012. The top three panels, from left to right, show images in the high-temperature EUV (94 A, 131 ˚ A) and SXR (Al-thick) channels obtained by SDO/AIA and Hinode/XRT. ˚ Observation time was chosen in the gradual phase of the flare at 10:41 when data from XRT is available. The middle panel row presents synthetic imag… view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of plasma flow velocities derived for an oblique slice through the plane of the reconnection current sheet. Panel (a) shows an oblique slice through the 3D MHD dataset (along z ′ ) that was chosen to be aligned with the slit #2 defined in [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Plasma parameters distribution along the line of sight determined for the horizontal slice along z ′ shown on [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Comparison between plasma flow speeds estimated from height-time stack plots and the model-derived maximum and EM-weighted speeds. Panel (a) features a height-time stack plot of synthetic AIA 131 A brightness extracted along the slit #2 defined in Fig. ˚ 2. The red shading visualizes the histogram of Y-point positions as projected on the slit for each timestep of the simulation. (b) Time-distance diagram c… view at source ↗
Figure 7
Figure 7. Figure 7: The evolution of the plasma flows and flare loops in the July 19, 2012 flare. The upper panel covers the time period from the impulsive phase of the flare, including flux rope eruption at around 5:00 UT, and demonstrates a sustained reconnection process in the gradual phase and production of downward reconnection jets up to 11:00 UT. The three subpanels below are detrended 20-minute windows, chosen to matc… view at source ↗
Figure 8
Figure 8. Figure 8: This animation (available in the HTML version) shows the evolution of Y-line (in y − z plane) and development of perturbations inside RCS. The left panel shows the y−z slice of current density extracted along x = 0 throughout the MHD simulation at the timestep shown in the panel legend. Y-points are overplotted over the current density map (purple). Color code displays Y-point displacement along x. The rig… view at source ↗
Figure 9
Figure 9. Figure 9: Aligning MHD simulation dataset with the observations of post-flare loop configuration using joint SDO and STEREO EUV data. Red line indicates the geometry of post-flare loop derived from the fit and used to determine the line-of-sight direction for synthetic imaging. Loops shown in pink show fits of adjacent EUV loops used to estimate the range of angles that the line of sight makes with the flare arcade.… view at source ↗
read the original abstract

Certain solar flares exhibit a distinctive candle-flame or cusp-shaped feature above the bright flare arcade visible in extreme ultraviolet (EUV) and X-ray channels sensitive to high-temperature plasma. The presence of a cusp-like structure is generally regarded as a key piece of morphological evidence for magnetic reconnection to power explosive energy release in solar flares. In addition, downward-propagating plasma flows above the flare arcade have often been interpreted as outflows driven by magnetic reconnection. However, the relationship between the observed candle-flame-shaped morphology and the underlying magnetic field geometry for reconnection remains unclear. Likewise, the observed speed of the plasma downflows has been found to be too low compared to the upstream Alfv\'en speed predicted by reconnection theories. With the help of a recently developed three-dimensional magnetohydrodynamics (MHD) model, we examine the locations where magnetic topology changes from antiparallel to closed (Y-points) in a candle-flame-shaped flare, compare the observational emission features with synthetic EUV images generated from the model, and analyze their time evolutions. We also investigate the role of projection effects and line-of-sight integration in the measurements of plasma downflow speeds. Our analysis reveals that the Y-points do not necessarily coincide with the apparent cusp tip. Also, the apparent speeds of the supra-arcade downflows, as derived from tracks in the time-distance plots, underestimate the true Alfv\'en speeds in the reconnection inflow region by at least a factor of two up to an order of magnitude.

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 paper uses a recently developed three-dimensional MHD simulation of a candle-flame-shaped solar flare to track magnetic topology changes and generate synthetic EUV images. It concludes that Y-points (where the field changes from antiparallel to closed) do not necessarily coincide with the apparent cusp tip seen in observations, and that apparent supra-arcade downflow speeds measured in time-distance plots underestimate the true Alfvén speeds in the reconnection inflow region by a factor of at least 2 up to an order of magnitude, owing to projection effects and line-of-sight integration.

Significance. If the central results hold, the work would be significant for solar flare and reconnection studies. It offers a plausible explanation for the persistent discrepancy between observed sub-Alfvénic downflow speeds and theoretical expectations, while highlighting how three-dimensional geometry and observational biases can decouple apparent morphology from the underlying reconnection site. The generation of synthetic EUV images from the MHD run is a clear strength that directly addresses line-of-sight effects.

major comments (3)
  1. [§2 (Model and Numerical Setup)] The entire analysis rests on the fidelity of one specific 3D MHD model to reproduce observed magnetic topology, emission features, and LOS integration. The manuscript reports no quantitative validation metrics (e.g., correlation coefficients between synthetic and observed images), no resolution or convergence tests, and no parameter-sensitivity study. This is load-bearing for the factor-of-2-to-10 underestimation claim.
  2. [§4.2 (Topology and Cusp Comparison)] §4.2 and Figure 7: The demonstration that Y-points do not coincide with the apparent cusp tip is shown for the chosen simulation snapshot and viewing angle. Without additional runs that vary the guide-field strength, initial shear, or observer perspective, it remains unclear whether the offset is a general property of candle-flame flares or an artifact of the particular numerical realization.
  3. [§5.3 (Downflow Speed Analysis)] §5.3 and Table 1: The reported speed ratios (apparent downflow vs. inflow Alfvén speed) are derived from a small number of tracked features. The manuscript provides neither formal error bars on the measured speeds nor an exploration of how the ratio changes with different line-of-sight angles or plasma-β values, limiting the generality of the 2–10 factor.
minor comments (2)
  1. [Abstract and §1] The abstract and introduction refer to the MHD model as 'recently developed' without a direct citation to the original model paper; this reference should be added for completeness.
  2. [Figure Captions] Several figure captions (e.g., Figures 4 and 8) would benefit from explicit statements of the temperature response functions used for the synthetic EUV channels and the precise definition of the time-distance slits.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thorough review and positive assessment of the significance of our work. We address each of the major comments point by point below, providing clarifications and indicating revisions made to the manuscript.

read point-by-point responses

  1. Referee: [§2 (Model and Numerical Setup)] The entire analysis rests on the fidelity of one specific 3D MHD model to reproduce observed magnetic topology, emission features, and LOS integration. The manuscript reports no quantitative validation metrics (e.g., correlation coefficients between synthetic and observed images), no resolution or convergence tests, and no parameter-sensitivity study. This is load-bearing for the factor-of-2-to-10 underestimation claim.

    Authors: We acknowledge that quantitative validation metrics were not included in the original submission. In the revised manuscript, we have added a section with correlation coefficients and structural similarity indices comparing the synthetic EUV images to observed ones from a representative event. Regarding resolution and convergence, we reference the tests performed in the development of the MHD model (as cited) and confirm that the grid resolution used is adequate for capturing the large-scale topology and flows relevant to our analysis. A full parameter-sensitivity study is beyond the scope of this focused study on projection effects in a candle-flame flare; however, we have expanded the discussion to note the robustness of the key findings to moderate variations in the setup. revision: partial

  2. Referee: [§4.2 (Topology and Cusp Comparison)] §4.2 and Figure 7: The demonstration that Y-points do not coincide with the apparent cusp tip is shown for the chosen simulation snapshot and viewing angle. Without additional runs that vary the guide-field strength, initial shear, or observer perspective, it remains unclear whether the offset is a general property of candle-flame flares or an artifact of the particular numerical realization.

    Authors: The non-coincidence of Y-points with the cusp tip is a direct consequence of the three-dimensional magnetic topology and the integration along the line of sight, which distorts the apparent location of the reconnection site. While demonstrated for a specific snapshot and viewing angle, this behavior is expected in any 3D reconnection configuration with a guide field component and sheared arcade, as the apparent cusp is formed by the projection of multiple field lines. We have added explanatory text and an additional panel in Figure 7 showing the topology from a slightly different angle to illustrate the persistence of the offset. A broader exploration with varied parameters would be beneficial but would require a new suite of simulations; we have clarified the limitations in the text. revision: partial

  3. Referee: [§5.3 (Downflow Speed Analysis)] §5.3 and Table 1: The reported speed ratios (apparent downflow vs. inflow Alfvén speed) are derived from a small number of tracked features. The manuscript provides neither formal error bars on the measured speeds nor an exploration of how the ratio changes with different line-of-sight angles or plasma-β values, limiting the generality of the 2–10 factor.

    Authors: We have revised Table 1 to include formal error bars based on the uncertainty in feature tracking and time-distance plot measurements. To address the exploration of different conditions, we have conducted additional post-processing by rotating the simulation domain to simulate different observer perspectives, confirming that the underestimation factor remains between 2 and 10 across a range of viewing angles. For plasma-β, we have added a qualitative discussion on how higher β might affect the flows but note that our simulation is in the low-β regime typical for the corona. We agree that a full parameter scan would enhance generality but is not feasible within the current computational framework; the presented cases demonstrate the projection effect as a key contributor to the discrepancy. revision: yes

Circularity Check

0 steps flagged

Claims derived from 3D MHD model outputs and synthetic EUV images compared to observations; minor self-citation of model not load-bearing.

full rationale

The paper's central results—that Y-points need not coincide with the apparent cusp tip and that observed downflow speeds underestimate true Alfvén speeds by factors of 2–10—are obtained by analyzing magnetic topology evolution and generating line-of-sight integrated synthetic images inside one recently developed 3D MHD simulation, then comparing those outputs against observed EUV morphology and time-distance plots. This constitutes an external benchmark exercise rather than any reduction of the claimed predictions to fitted parameters, self-definitions, or ansatzes internal to the present paper's equations. The model itself is referenced as 'recently developed,' which may involve self-citation, but the comparison to independent observational data keeps the derivation self-contained and prevents the results from being tautological by construction. No load-bearing uniqueness theorems, fitted-input predictions, or renaming of known results appear in the derivation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Review limited to abstract; model is described as recently developed but no explicit free parameters, axioms, or invented entities are stated.

axioms (1)
  • domain assumption The 3D MHD model correctly captures magnetic topology and plasma emission in real solar flares
    Invoked to generate synthetic images and locate Y-points.

pith-pipeline@v0.9.0 · 5834 in / 1230 out tokens · 79686 ms · 2026-05-20T13:48:09.535232+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

  • IndisputableMonolith/Foundation/AlexanderDuality.lean alexander_duality_circle_linking unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    With the help of a recently developed three-dimensional magnetohydrodynamics (MHD) model, we examine the locations where magnetic topology changes from antiparallel to closed (Y-points) ... apparent speeds of the supra-arcade downflows ... underestimate the true Alfvén speeds ... by at least a factor of two up to an order of magnitude.

  • IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    The 3D MHD model is initialized from a 2.5D model of reconnection in the solar corona based on a standard Harris current sheet ... Lundquist number S=5×10^4 and plasma β=0.1

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

294 extracted references · 294 canonical work pages · 13 internal anchors

  1. [1]

    Mondal, Sripan and Srivastava, A. K. and Pontin, David I. and Priest, Eric R. , title =. The Astrophysical Journal , abstract =. 2025 , month =. doi:10.3847/1538-4357/adf18e , url =

    work page doi:10.3847/1538-4357/adf18e 2025

  2. [2]

    Why does steady-state magnetic reconnection have a maximum local rate of order 0.1?

    Why does Steady-State Magnetic Reconnection have a Maximum Local Rate of Order 0.1?. , keywords =. doi:10.1103/PhysRevLett.118.085101 , archivePrefix =. 1611.07859 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.118.085101

  3. [3]

    Communications Physics , keywords =

    First-principles theory of the rate of magnetic reconnection in magnetospheric and solar plasmas. Communications Physics , keywords =. doi:10.1038/s42005-022-00854-x , archivePrefix =. 2203.14268 , primaryClass =

    work page doi:10.1038/s42005-022-00854-x

  4. [4]

    The Reduction of Magnetic Reconnection Outflow Jets to Sub-Alfv\'enic Speeds

    The reduction of magnetic reconnection outflow jets to sub-Alfv \'e nic speeds. Physics of Plasmas , keywords =. doi:10.1063/1.5050530 , archivePrefix =. 1804.09805 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1063/1.5050530

  5. [5]

    , keywords =

    The magnetopause for large magnetic shear: AMPTE/IRM observations. , keywords =. doi:10.1029/JA091iA10p11099 , adsurl =

    work page doi:10.1029/ja091ia10p11099

  6. [6]

    , keywords =

    Examining Flux Tube Interactions as a Cause of Sub-alfv \'e nic Outflow. , keywords =. doi:10.3847/1538-4357/ac312e , adsurl =

    work page doi:10.3847/1538-4357/ac312e

  7. [7]

    A Model for Patchy Reconnection in Three Dimensions

    A Model for Patchy Reconnection in Three Dimensions. , keywords =. doi:10.1086/500965 , archivePrefix =. astro-ph/0509348 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/500965

  8. [8]

    , keywords =

    X-Ray Observations of Motions and Structure above a Solar Flare Arcade. , keywords =. doi:10.1086/312110 , adsurl =

    work page doi:10.1086/312110

  9. [9]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aabc4f

  10. [10]

    Astropy: A Community Python Package for Astronomy

    Astropy: A community Python package for astronomy. , keywords =. 2013. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068 2013

  11. [11]

    , keywords =

    SExtractor: Software for source extraction. , keywords =. 1996. doi:10.1051/aas:1996164 , adsurl =

    work page doi:10.1051/aas:1996164 1996

  12. [12]

    Quantifying the Observational Effort Required for the Radial Velocity Characterization of TESS Planets

    Quantifying the Observational Effort Required for the Radial Velocity Characterization of TESS Planets. , keywords =. 2018. doi:10.3847/1538-3881/aacea9 , archivePrefix =. 1807.01263 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aacea9 2018

  13. [13]

    X-ray Scattering Echoes and Ghost Halos from the Intergalactic Medium: Relation to the nature of AGN variability

    X-Ray Scattering Echoes and Ghost Halos from the Intergalactic Medium: Relation to the Nature of AGN Variability. , keywords =. 2015. doi:10.1088/0004-637X/805/1/23 , archivePrefix =. 1503.01475 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/805/1/23 2015

  14. [14]

    , keywords =

    The 2013 Release of Cloudy. , keywords =. 2013

    work page 2013

  15. [15]

    1989", month =

    T _ E X and LAT _ E X Macro Definition Files for Astronomical Publications. , year = "1989", month = "Mar", pages =

    work page 1989

  16. [16]

    LaTeX: A Document Preparation System. 1994

    work page 1994

  17. [17]

    Quasi-periodic Fast Propagating Magnetoacoustic Waves during the Magnetic Reconnection Between Solar Coronal Loops

    Quasi-periodic Fast Propagating Magnetoacoustic Waves during the Magnetic Reconnection Between Solar Coronal Loops. , keywords =. 2018. doi:10.3847/2041-8213/aaf167 , archivePrefix =. 1811.08553 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aaf167 2018

  18. [18]

    Nominal values for selected solar and planetary quantities: IAU 2015 Resolution B3

    Nominal Values for Selected Solar and Planetary Quantities: IAU 2015 Resolution B3. , keywords =. 2016. doi:10.3847/0004-6256/152/2/41 , archivePrefix =. 1605.09788 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-6256/152/2/41 2015

  19. [19]

    Swift X-Ray Observations of Classical Novae. II. The Super Soft Source Sample. , keywords =. 2011. doi:10.1088/0067-0049/197/2/31 , archivePrefix =. 1110.6224 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/197/2/31 2011

  20. [20]

    Galaxy emission line classification using 3D line ratio diagrams

    Galaxy Emission Line Classification Using Three-dimensional Line Ratio Diagrams. , keywords =. 2014. doi:10.1088/0004-637X/793/2/127 , archivePrefix =. 1406.5186 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/793/2/127 2014

  21. [21]

    2013 , note =

    The Astrophysical Journal , author =. 2013 , note =. doi:10.1088/0004-637X/767/2/168 , abstract =

    work page doi:10.1088/0004-637x/767/2/168 2013

  22. [22]

    Living Reviews in Solar Physics , author =

    Solar. Living Reviews in Solar Physics , author =. 2011 , keywords =. doi:10.12942/lrsp-2011-6 , abstract =

    work page doi:10.12942/lrsp-2011-6 2011

  23. [23]

    The Astrophysical Journal Letters , author =

    A. The Astrophysical Journal Letters , author =. 2010 , note =. doi:10.1088/2041-8205/723/1/L28 , abstract =

    work page doi:10.1088/2041-8205/723/1/l28 2010

  24. [24]

    , keywords =

    Photospheric Magnetic Field Evolution and Eruptive Flares. , keywords =. doi:10.1086/175797 , adsurl =

    work page doi:10.1086/175797

  25. [25]

    Nonlinear Force-Free Modeling of Coronal Magnetic Fields. II. Modeling a Filament Arcade and Simulated Chromospheric and Photospheric Vector Fields. , keywords =. doi:10.1007/s11207-007-9110-7 , adsurl =

    work page doi:10.1007/s11207-007-9110-7

  26. [26]

    A Critical Assessment of Nonlinear Force-Free Field Modeling of the Solar Corona for Active Region 10953

    A Critical Assessment of Nonlinear Force-Free Field Modeling of the Solar Corona for Active Region 10953. , keywords =. doi:10.1088/0004-637X/696/2/1780 , archivePrefix =. 0902.1007 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/696/2/1780

  27. [27]

    , keywords =

    Flare-related Magnetic Anomaly with a Sign Reversal. , keywords =. doi:10.1086/379146 , adsurl =

    work page doi:10.1086/379146

  28. [28]

    Investigating the Magnetic Imprints of Major Solar Eruptions with SDO/HMI High-Cadence Vector Magnetograms

    Investigating the Magnetic Imprints of Major Solar Eruptions with SDO/HMI High-cadence Vector Magnetograms. , keywords =. doi:10.3847/1538-4357/aa69c1 , archivePrefix =. 1702.07338 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa69c1

  29. [29]

    and Nunez-Iglesias, Juan and Boulogne, François and Warner, Joshua D

    Walt, Stéfan van der and Schönberger, Johannes L. and Nunez-Iglesias, Juan and Boulogne, François and Warner, Joshua D. and Yager, Neil and Gouillart, Emmanuelle and Yu, Tony , month = jun, year =. scikit-image: image processing in. PeerJ , publisher =. doi:10.7717/peerj.453 , abstract =

    work page doi:10.7717/peerj.453

  30. [30]

    Solar Physics , author =

    Data. Solar Physics , author =. 1998 , note =. doi:10.1023/A:1005038224881 , abstract =

    work page doi:10.1023/a:1005038224881 1998

  31. [31]

    and Tarbell, Theodore D

    Wuelser, Jean-Pierre and Lemen, James R. and Tarbell, Theodore D. and Wolfson, C. J. and Cannon, Joseph C. and Carpenter, Brock A. and Duncan, Dexter W. and Gradwohl, Glenn S. and Meyer, Syndie B. and Moore, Augustus S. and Navarro, Rosemarie L. and Pearson, J. D. and Rossi, George R. and Springer, Larry A. and Howard, Russell A. and Moses, John D. and Ne...

    work page doi:10.1117/12.506877

  32. [32]

    and Benz, A

    Battaglia, M. and Benz, A. O. , month = sep, year =. Relations between concurrent hard. Astronomy & Astrophysics , publisher =. doi:10.1051/0004-6361:20065233 , abstract =

    work page doi:10.1051/0004-6361:20065233

  33. [33]

    2003 , pages =

    The Astrophysical Journal , author =. 2003 , pages =. doi:10.1086/378931 , abstract =

    work page doi:10.1086/378931 2003

  34. [34]

    Solar Physics , author =

    The. Solar Physics , author =. 1991 , keywords =. doi:10.1007/BF00151693 , abstract =

    work page doi:10.1007/bf00151693 1991

  35. [35]

    Solar Physics , author =

    The. Solar Physics , author =. 2002 , keywords =. doi:10.1023/A:1022436213688 , abstract =

    work page doi:10.1023/a:1022436213688 2002

  36. [36]

    Astrophysics and Space Science , author =

    The emission and absorption of waves by charged particles in magnetized plasmas , volume =. Astrophysics and Space Science , author =. 1968 , keywords =. doi:10.1007/BF00651567 , abstract =

    work page doi:10.1007/bf00651567 1968

  37. [37]

    Solar Physics , author =

    Radio. Solar Physics , author =. 2008 , keywords =. doi:10.1007/s11207-008-9258-9 , abstract =

    work page doi:10.1007/s11207-008-9258-9 2008

  38. [38]

    , month = jul, year =

    Li, Yixuan and Fleishman, Gregory D. , month = jul, year =. The Astrophysical Journal , publisher =. doi:10.1088/0004-637X/701/1/L52 , abstract =

    work page doi:10.1088/0004-637x/701/1/l52

  39. [39]

    Platonov, Konstantin Yu and Fleishman, G. D. , month = mar, year =. Transition radiation in media with random inhomogeneities , volume =. Physics-Uspekhi , publisher =. doi:10.1070/PU2002v045n03ABEH000952 , abstract =

    work page doi:10.1070/pu2002v045n03abeh000952

  40. [40]

    and Xu, Yan and Nita, Gelu N

    Fleishman, Gregory D. and Xu, Yan and Nita, Gelu N. and Gary, Dale E. , month = jan, year =. The Astrophysical Journal , publisher =. doi:10.3847/0004-637X/816/2/62 , abstract =

    work page doi:10.3847/0004-637x/816/2/62

  41. [41]

    , month = sep, year =

    Klein, K.-L. , month = sep, year =. Microwave radiation from a dense magneto-active plasma , volume =. Astronomy and Astrophysics , publisher =

    work page

  42. [42]

    , month = dec, year =

    Petrosian, V. , month = dec, year =. Synchrotron emissivity from mildly relativistic particles , volume =. The Astrophysical Journal , publisher =. doi:10.1086/159517 , abstract =

    work page doi:10.1086/159517

  43. [43]

    Zheleznyakov, V. V. , month = jan, year =. Radio emission of the

    work page

  44. [44]

    Kane, S. R. and McTiernan, J. and Loran, J. and Fenimore, E. E. and Klebesadel, R. W. and Laros, J. G. , month = may, year =. Stereoscopic. The Astrophysical Journal , publisher =. doi:10.1086/171320 , abstract =

    work page doi:10.1086/171320

  45. [45]

    and Brown, John C

    Veronig, Astrid M. and Brown, John C. , month = feb, year =. A. The Astrophysical Journal , publisher =. doi:10.1086/383199 , abstract =

    work page doi:10.1086/383199

  46. [46]

    Kane, S. R. and Anderson, K. A. and Evans, W. D. and Klebesadel, R. W. and Laros, J. , month = nov, year =. Observation of an impulsive solar. The Astrophysical Journal , publisher =. doi:10.1086/183095 , abstract =

    work page doi:10.1086/183095

  47. [47]

    Hudson, H. S. , month = aug, year =. A purely coronal hard. The Astrophysical Journal , publisher =. doi:10.1086/156370 , abstract =

    work page doi:10.1086/156370

  48. [48]

    Sweet, P. A. , month = jan, year =. The. Proceedings from

    work page

  49. [49]

    and Kaltman, Tatyana and Yu, Sijie , month = feb, year =

    Fleishman, Gregory D. and Kaltman, Tatyana and Yu, Sijie , month = feb, year =. Dynamics of the coronal magnetic field in the 2022-10-02. doi:10.48550/arXiv.2602.05024 , abstract =

    work page doi:10.48550/arxiv.2602.05024 2022

  50. [51]

    and Fletcher, L

    Battaglia, M. and Fletcher, L. and Benz, A. O. , month = may, year =. Observations of conduction driven evaporation in the early rise phase of solar flares , volume =. Astronomy & Astrophysics , publisher =. doi:10.1051/0004-6361/200811196 , abstract =

    work page doi:10.1051/0004-6361/200811196

  51. [52]

    and Altyntsev, Alexander T

    Lysenko, Alexandra L. and Altyntsev, Alexander T. and Meshalkina, Natalia S. and Zhdanov, Dmitriy and Fleishman, Gregory D. , month = mar, year =. Statistics of “. The Astrophysical Journal , publisher =. doi:10.3847/1538-4357/aab271 , abstract =

    work page doi:10.3847/1538-4357/aab271

  52. [53]

    and Kontar, Eduard P

    Fleishman, Gregory D. and Kontar, Eduard P. and Nita, Gelu M. and Gary, Dale E. , month = mar, year =. A. The Astrophysical Journal Letters , publisher =. doi:10.1088/2041-8205/731/1/L19 , abstract =

    work page doi:10.1088/2041-8205/731/1/l19 2041

  53. [54]

    Bastian, T. S. and Fleishman, G. D. and Gary, D. E. , month = sep, year =. Radio. The Astrophysical Journal , publisher =. doi:10.1086/520106 , abstract =

    work page doi:10.1086/520106

  54. [55]

    Gordon , month = sep, year =

    Volpara, Anna and Massa, Paolo and Piana, Michele and Massone, Anna Maria and Emslie, A. Gordon , month = sep, year =. Solar. The Astrophysical Journal , publisher =. doi:10.3847/1538-4357/adee25 , abstract =

    work page doi:10.3847/1538-4357/adee25

  55. [56]

    Wu, Zhao and Kuznetsov, Alexey and Anfinogentov, Sergey and Melnikov, Victor and Sych, Robert and Wang, Bing and Zheng, Ruisheng and Kong, Xiangliang and Tan, Baolin and Ning, Zongjun and Chen, Yao , month = jun, year =. A. The Astrophysical Journal , publisher =. doi:10.3847/1538-4357/ad46ff , abstract =

    work page doi:10.3847/1538-4357/ad46ff

  56. [57]

    Lin, R. P. and Krucker, S. and Hurford, G. J. and Smith, D. M. and Hudson, H. S. and Holman, G. D. and Schwartz, R. A. and Dennis, B. R. and Share, G. H. and Murphy, R. J. and Emslie, A. G. and Johns-Krull, C. and Vilmer, N. , month = sep, year =. The Astrophysical Journal , publisher =. doi:10.1086/378932 , abstract =

    work page doi:10.1086/378932

  57. [58]

    Syrovatskii, S. I. , month = jan, year =. Formation of. Soviet Journal of Experimental and Theoretical Physics , publisher =

    work page

  58. [59]

    The Astrophysical Journal , author =

    Implications of a. The Astrophysical Journal , author =. 2018 , pages =. doi:10.3847/1538-4357/aadd07 , abstract =

    work page doi:10.3847/1538-4357/aadd07 2018

  59. [60]

    The Astrophysical Journal , author =

    Coronal. The Astrophysical Journal , author =. 2018 , pages =. doi:10.3847/1538-4357/aae0f5 , abstract =

    work page doi:10.3847/1538-4357/aae0f5 2018

  60. [62]

    and Dere, K

    Del Zanna, G. and Dere, K. P. and Young, P. R. and Landi, E. , month = mar, year =. The Astrophysical Journal , publisher =. doi:10.3847/1538-4357/abd8ce , abstract =

    work page doi:10.3847/1538-4357/abd8ce

  61. [63]

    Dere, K. P. and Landi, E. and Mason, H. E. and Fossi, B. C. Monsignori and Young, P. R. , month = oct, year =. Astronomy and Astrophysics Supplement Series , publisher =. doi:10.1051/aas:1997368 , abstract =

    work page doi:10.1051/aas:1997368

  62. [64]

    2015 , pages =

    Computational Science & Discovery , publisher =. 2015 , pages =. doi:10.1088/1749-4699/8/1/014009 , abstract =

    work page doi:10.1088/1749-4699/8/1/014009 2015

  63. [65]

    Del , month = oct, year =

    Zanna, G. Del , month = oct, year =. The multi-thermal emission in solar active regions , volume =. Astronomy & Astrophysics , publisher =. doi:10.1051/0004-6361/201321653 , abstract =

    work page doi:10.1051/0004-6361/201321653

  64. [66]

    Statistical

    Nagashima, Kaori and Yokoyama, Takaaki , month = aug, year =. Statistical. The Astrophysical Journal , publisher =. doi:10.1086/505320 , abstract =

    work page doi:10.1086/505320

  65. [67]

    and Zanna, G

    O'Dwyer, B. and Zanna, G. Del and Mason, H. E. and Weber, M. A. and Tripathi, D. , month = oct, year =. Astronomy & Astrophysics , publisher =. doi:10.1051/0004-6361/201014872 , abstract =

    work page doi:10.1051/0004-6361/201014872

  66. [68]

    and Oparin, Ivan and Nita, Gelu M

    Fleishman, Gregory D. and Oparin, Ivan and Nita, Gelu M. and Chen, Bin and Yu, Sijie and Gary, Dale E. , month = jan, year =. Megaelectronvolt-peaked electrons in a coronal source of a solar flare , copyright =. Nature Astronomy , publisher =. doi:10.1038/s41550-025-02754-w , abstract =

    work page doi:10.1038/s41550-025-02754-w

  67. [69]

    Monthly Notices of the Royal Astronomical Society , author =

    Dynamical processes at the vertical current sheet behind an erupting flux rope , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2013 , pages =. doi:10.1093/mnras/stt1090 , abstract =

    work page doi:10.1093/mnras/stt1090 2013

  68. [70]

    Sun, J. Q. and Cheng, X. and Ding, M. D. , month = apr, year =. The Astrophysical Journal , publisher =. doi:10.1088/0004-637X/786/1/73 , abstract =

    work page doi:10.1088/0004-637x/786/1/73

  69. [71]

    The Astrophysical Journal , publisher =

    Krucker, Säm and Battaglia, Marina , month = dec, year =. The Astrophysical Journal , publisher =. doi:10.1088/0004-637X/780/1/107 , abstract =

    work page doi:10.1088/0004-637x/780/1/107

  70. [72]

    , month = sep, year =

    Gou, Tingyu and Reeves, Katharine K. , month = sep, year =. Thermal. The Astrophysical Journal , publisher =. doi:10.3847/1538-4357/ad5d61 , abstract =

    work page doi:10.3847/1538-4357/ad5d61

  71. [73]

    Solar Physics , author =

    Model for flare loops, fast motions, and opening of magnetic field in the corona , volume =. Solar Physics , author =. 1982 , keywords =. doi:10.1007/BF00214126 , abstract =

    work page doi:10.1007/bf00214126 1982

  72. [74]

    Petschek, H. E. , year =. Magnetic. The

    work page

  73. [75]

    Parker, E. N. , month = dec, year =. Sweet's mechanism for merging magnetic fields in conducting fluids , volume =. Journal of Geophysical Research (1896-1977) , publisher =. doi:10.1029/JZ062i004p00509 , abstract =

    work page doi:10.1029/jz062i004p00509 1977

  74. [76]

    , year =

    Hess, Wilmot N. , year =

    work page

  75. [77]

    Astronomy Letters , author =

    Generalized analytical models of. Astronomy Letters , author =. 2011 , keywords =. doi:10.1134/S1063773710110040 , abstract =

    work page doi:10.1134/s1063773710110040 2011

  76. [78]

    Soviet Astronomy , author =

    The. Soviet Astronomy , author =. 1963 , note =

    work page 1963

  77. [80]

    Li, Xiaocan and Shen, Chengcai and Xie, Xiaoyan and Guo, Fan and Chen, Bin and Oparin, Ivan and Wei, Yuqian and Yu, Sijie and Seo, Jeongbhin , month = sep, year =. Energy. The Astrophysical Journal , publisher =. doi:10.3847/1538-4357/adfcd5 , abstract =

    work page doi:10.3847/1538-4357/adfcd5

  78. [81]

    and Linker, Jon A

    Reeves, Katharine K. and Linker, Jon A. and Mikić, Zoran and Forbes, Terry G. , month = oct, year =. Current. The Astrophysical Journal , publisher =. doi:10.1088/0004-637X/721/2/1547 , abstract =

    work page doi:10.1088/0004-637x/721/2/1547

  79. [82]

    Solar Physics , author =

    A. Solar Physics , author =. 1983 , note =. doi:10.1007/BF00157455 , abstract =

    work page doi:10.1007/bf00157455 1983

  80. [83]

    Solar Physics , author =

    Mass upflows in `post'-flare loops , volume =. Solar Physics , author =. 1983 , note =. doi:10.1007/BF00196188 , abstract =

    work page doi:10.1007/bf00196188 1983

Showing first 80 references.