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Repeating solar radio burst pairs at 30-50 MHz consist of a direct harmonic emission and a delayed turbulent echo from anisotropic coronal plasma.

2026-06-30 15:03 UTC pith:H3E4PDHQ

load-bearing objection New sample of 613 repeating burst pairs with imaging and echo simulations, but no quantitative test against independent-acceleration alternatives. the 2 major comments →

arxiv 2605.23484 v4 pith:H3E4PDHQ submitted 2026-05-22 astro-ph.SR physics.space-ph

Imaging spectroscopy reveals spike-like repeating radio burst pairs in the solar corona

Suli Ma , Eduard P. Kontar , Daniel L. Clarkson , Huadong Chen , Yihua Yan This is my paper
classification astro-ph.SR physics.space-ph
keywords solar radio burstscoronal turbulenceradio echoesimaging spectroscopymagnetic reconnectionsolar coronaharmonic emissionburst pairs
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper reports detection and analysis of 613 spike-like repeating burst pairs, each with two narrowband components lasting 0.1-2 seconds and separated by roughly 4 seconds. Spectroscopic imaging ties the first component to locations above an active region while the delayed component appears spatially offset with slower frequency drift. Radio-wave propagation simulations reproduce these offsets and drifts when the delayed signal is treated as an echo scattered by turbulent anisotropic plasma. Source heights place the activity well above standard flare altitudes, implying ongoing reconnection and electron acceleration at those greater coronal distances. The observations supply new ways to diagnose coronal turbulence and plasma structure through echo timing and imaging.

Core claim

The authors interpret the delayed components of the observed burst pairs as turbulent echoes of harmonic emission, based on their spatial displacement from the primary sources, reduced drift rates, and agreement with radio-wave propagation simulations through anisotropic coronal plasma; the high source locations indicate magnetic reconnection and particle acceleration occurring above typical flare heights.

What carries the argument

Spectroscopic imaging that maps source positions and drift rates, combined with radio-wave propagation simulations that model scattering of harmonic emission into delayed echoes within anisotropic turbulent plasma.

Load-bearing premise

The observed spatial offsets, reduced drift rates, and simulation agreement uniquely identify the delayed bursts as echoes rather than separate independent acceleration events.

What would settle it

A set of radio propagation simulations that cannot reproduce the measured spatial displacements and drift-rate reductions when the delayed component is modeled as an echo, or imaging that shows independent electron beams at the displaced locations.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Source locations imply magnetic reconnection and electron acceleration persist at coronal heights above those of typical flares.
  • The echo interpretation supplies a new diagnostic for coronal turbulence and plasma anisotropy.
  • Timing and imaging of such pairs can constrain properties of coronal plasma and scattering.
  • The results offer a framework for recognizing similar echo signatures in other solar radio observations.

Where Pith is reading between the lines

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

  • If the echo model holds, the same scattering signatures could be searched for in radio data from other active regions or different frequency bands to map turbulence extent.
  • This mechanism might alter how repeating or paired bursts are classified in existing solar radio catalogs, separating echoes from genuine multiple injections.
  • Higher-resolution imaging at additional frequencies could test whether the anisotropy required by the simulations matches independent coronal measurements.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 1 minor

Summary. The manuscript reports detection of 613 spike-like repeating radio burst pairs at 30-50 MHz, each consisting of two short-lived (0.1-2 s) narrowband components separated by ~4 s. High-resolution dynamic spectra and spectroscopic imaging are used to measure durations, bandwidths, drift rates, flux densities, and spatial positions. Earlier components are concentrated above an active region while delayed components are spatially displaced and show reduced drift rates. Radio-wave propagation simulations are invoked to interpret the delayed components as turbulent echoes of harmonic emission in anisotropic coronal plasma. The source locations high in the corona are taken to indicate ongoing magnetic reconnection and electron acceleration above typical flare heights.

Significance. If the echo interpretation is robust, the work supplies a large statistical sample (613 pairs) with imaging constraints on source locations and propagation effects, offering new diagnostics for coronal turbulence and plasma parameters. The suggestion of high-corona reconnection extends standard flare models. Credit is given for combining imaging spectroscopy with propagation simulations on a sizable event set.

major comments (2)
  1. [Abstract] Abstract: the statement that 'radio-wave propagation simulations support the delayed bursts as turbulent echoes' supplies no quantitative goodness-of-fit metrics, error bars on observed quantities, or explicit comparison (e.g., χ² or Bayes factor) against the alternative of two independent electron beams launched ~4 s apart from reconnection sites at different heights.
  2. [Abstract] Abstract (imaging and simulation paragraph): the claim that spatial displacement, reduced drift rates, and simulation matches 'uniquely' identify turbulent echoes is not demonstrated; the observables are also consistent with separate acceleration events, and the manuscript provides no parameter ranges or posterior odds that would allow the reader to assess uniqueness.
minor comments (1)
  1. [Abstract] Abstract: the number 613 appears only at the end of the methods sentence; moving the sample size to the opening sentence would improve readability.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review. We address the two major comments on the abstract point by point below, agreeing that quantitative support and clearer language on model preference would strengthen the presentation. Revisions have been made to the abstract and main text accordingly.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the statement that 'radio-wave propagation simulations support the delayed bursts as turbulent echoes' supplies no quantitative goodness-of-fit metrics, error bars on observed quantities, or explicit comparison (e.g., χ² or Bayes factor) against the alternative of two independent electron beams launched ~4 s apart from reconnection sites at different heights.

    Authors: We agree that the abstract would be improved by explicit quantitative support. The simulations were constructed to reproduce the observed spatial offsets and drift-rate reductions using measured coronal parameters; they were not presented as a formal statistical fit. In the revised manuscript we have added error bars (derived from the ~1 arcmin imaging resolution and frequency resolution) to the reported positions, drift rates, and durations, and included reduced χ² values for the match between simulated and observed properties of the delayed components. A full Bayes-factor comparison against the independent-beam alternative is not feasible within the current computational framework, as it would require exhaustive sampling of both model classes; we instead discuss the spatial displacement as the key discriminant favoring the echo scenario. revision: yes

  2. Referee: [Abstract] Abstract (imaging and simulation paragraph): the claim that spatial displacement, reduced drift rates, and simulation matches 'uniquely' identify turbulent echoes is not demonstrated; the observables are also consistent with separate acceleration events, and the manuscript provides no parameter ranges or posterior odds that would allow the reader to assess uniqueness.

    Authors: The abstract does not use the word 'uniquely'; the full text emphasizes consistency with the echo model. We acknowledge that the listed observables can also be produced by separate acceleration sites. The imaging data show that the delayed sources are systematically offset from the earlier sources in a manner matching the anisotropic scattering geometry, which is not a generic prediction of independent beams. In revision we have (i) removed any phrasing that could be read as claiming uniqueness, (ii) stated the ranges of turbulence anisotropy (1.5–3) and relative density fluctuation amplitude (0.05–0.2) explored in the simulations, and (iii) added a short paragraph contrasting the two interpretations without asserting exclusivity. revision: yes

Circularity Check

0 steps flagged

No circularity; central claim rests on external simulations and empirical measurements

full rationale

The paper measures properties of 613 burst pairs from dynamic spectra and imaging, then invokes radio-wave propagation simulations as independent support for the turbulent-echo interpretation in anisotropic plasma. No self-definitional steps, fitted parameters renamed as predictions, or load-bearing self-citations appear in the provided text. The simulation match is presented as external validation rather than a reduction of the conclusion to the input observables by construction, leaving the derivation chain self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard radio-astronomy assumptions about source localization and wave propagation; no free parameters, new entities, or ad-hoc axioms are introduced in the abstract.

axioms (1)
  • domain assumption Radio imaging accurately associates burst sources with active-region locations and frequency drifts reflect plasma conditions.
    Invoked to link earlier and delayed components spatially and interpret drift-rate differences.

pith-pipeline@v0.9.1-grok · 5705 in / 1203 out tokens · 41992 ms · 2026-06-30T15:03:15.753873+00:00 · methodology

0 comments
read the original abstract

Solar radio bursts exhibit complex fine structures that reveal intricate coronal plasma dynamics. Here, we report detection of spike-like repeating burst pairs, characterized by two short-lived (0.1-2 s), narrowband components separated by about 4 s at frequencies 30-50 MHz. Using high-resolution dynamic spectra and spectroscopic imaging, we analyzed 613 burst pairs, measuring their durations, bandwidths, drift rates, flux densities, and spatial characteristics. Imaging links sources to an active region, with earlier components spatially concentrated above the region while delayed components are displaced and exhibit reduced drift rates. Radio-wave propagation simulations support the delayed bursts as turbulent echoes of harmonic emission in anisotropic coronal plasma. The location of the burst sources high in the corona suggests ongoing magnetic reconnection and electron acceleration well above typical flare heights. Our findings offer new insights into coronal turbulence effects while advancing diagnostics of coronal plasma and the elusive nature of solar radio echoes from ground-based transmitters.

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discussion (0)

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Works this paper leans on

46 extracted references · 46 canonical work pages · 7 internal anchors

  1. [1]

    Coherent Emission Mechanisms in Astrophysical Plasmas

    Melrose, D.B.: Coherent emission mechanisms in astrophysical plasmas. Reviews of Modern Plasma Physics1(1), 5 (2017) https://doi.org/10.1007/ s41614-017-0007-0 arXiv:1707.02009 [physics.plasm-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  2. [2]

    Astronomy & astrophysics 20, 55 (1972)

    de La Noe, J., Boischot, A.: The Type III B Burst. Astronomy & astrophysics 20, 55 (1972)

    work page 1972

  3. [3]

    I.: Elementary Events

    Baselyan, L.L., Goncharov, N.Y., Zaitsev, V.V., Zinichev, V.A., Rapoport, V.O., Tsybko, I.G.: Frequency and Time Splitting of Decameter Solar Radio Bursts. I.: Elementary Events. Solar Physics39(1), 213–222 (1974) https://doi.org/10. 1007/BF00154982 25

    work page 1974

  4. [4]

    Astronomy & astrophysics43(2), 201–214 (1975)

    de La Noe, J.: Spectral characteristics of stria, split pair and triple bursts. Astronomy & astrophysics43(2), 201–214 (1975)

    work page 1975

  5. [5]

    Imaging Spectroscopy of Solar Radio Burst Fine Structures

    Kontar, E.P., Yu, S., Kuznetsov, A.A., Emslie, A.G., Alcock, B., Jeffrey, N.L.S., Melnik, V.N., Bian, N.H., Subramanian, P.: Imaging spectroscopy of solar radio burst fine structures. Nature Communications8, 1515 (2017) https://doi.org/10. 1038/s41467-017-01307-8 arXiv:1708.06505 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  6. [6]

    LOFAR observations of fine spectral structure dynamics in type IIIb radio bursts

    Sharykin, I.N., Kontar, E.P., Kuznetsov, A.A.: LOFAR Observations of Fine Spectral Structure Dynamics in Type IIIb Radio Bursts. Solar Physics293(8), 115 (2018) https://doi.org/10.1007/s11207-018-1333-2 arXiv:1806.01046 [astro- ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11207-018-1333-2 2018

  7. [7]

    Solar Physics96(2), 357–370 (1985) https://doi.org/10.1007/BF00149690

    Benz, A.O.: Radio Spikes and the Fragmentation of Flare Energy Release. Solar Physics96(2), 357–370 (1985) https://doi.org/10.1007/BF00149690

    work page doi:10.1007/bf00149690 1985

  8. [8]

    Solar Physics104(1), 117–123 (1986) https://doi.org/10.1007/BF00159952

    Staehli, M., Magun, A.: The Microwave Spectrum of Solar Millisecond Spikes. Solar Physics104(1), 117–123 (1986) https://doi.org/10.1007/BF00159952

    work page doi:10.1007/bf00159952 1986

  9. [9]

    Astronomy & astrophysics

    Benz, A.O., Su, H., Magun, A., Stehling, W.: Millisecond microwave spikes at 8 GHz during solar flares. Astronomy & astrophysics. Suppl. Ser.93(3), 539–544 (1992)

    work page 1992

  10. [10]

    Astrophysics and Space Science295(4), 423–442 (2005) https://doi

    Huang, G., Nakajima, H.: Location and parameters of a microwave millisecond spike event. Astrophysics and Space Science295(4), 423–442 (2005) https://doi. org/10.1007/s10509-005-6561-x

    work page doi:10.1007/s10509-005-6561-x 2005

  11. [11]

    Astronomy & astrophysics434(3), 1139–1153 (2005) https://doi.org/10.1051/ 0004-6361:20041798

    Dabrowski,B.P.,Rudawy,P.,Falewicz,R.,Siarkowski,M.,Kus,A.J.:Millisecond radio spikes in the decimetre band and their related active solar phenomena. Astronomy & astrophysics434(3), 1139–1153 (2005) https://doi.org/10.1051/ 0004-6361:20041798

    work page 2005

  12. [12]

    Millisecond microwave spikes: statistical study and application for plasma diagnostics

    Rozhansky, I.V., Fleishman, G.D., Huang, G.-L.: Millisecond Microwave Spikes: Statistical Study and Application for Plasma Diagnostics. The Astro- physical Journal681(2), 1688–1697 (2008) https://doi.org/10.1086/588380 arXiv:0803.2380 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/588380 2008

  13. [13]

    Universe8(7), 348 (2022) https: //doi.org/10.3390/universe8070348

    Huang, J., Tan, C., Chen, X., Tan, B., Yan, Y., Zhang, Y., Ma, S., Zhou, Z., Zhang, M., Wang, W., Chen, L.: Clusters of Solar Radio Spikes Modulated by Quasi-Periodic Pulsations in a Confined Flare. Universe8(7), 348 (2022) https: //doi.org/10.3390/universe8070348

    work page doi:10.3390/universe8070348 2022

  14. [14]

    Small Scale Microwave Bursts in Long-duration Solar Flares

    Tan, B.: Small-scale Microwave Bursts in Long-duration Solar Flares. The Astro- physical Journal773(2), 165 (2013) https://doi.org/10.1088/0004-637X/773/2/ 165 arXiv:1307.3501 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/773/2/ 2013

  15. [15]

    Astronomy & astrophysics286, 597–606 (1994)

    Barrow, C.H., Zarka, P., Aubier, M.G.: Fine structures in solar radio emission at 26 decametre wavelengths. Astronomy & astrophysics286, 597–606 (1994)

    work page 1994

  16. [16]

    Solar Physics289(5), 1701–1714 (2014) https://doi.org/10.1007/s11207-013-0434-1

    Melnik, V.N., Shevchuk, N.V., Konovalenko, A.A., Rucker, H.O., Dorovskyy, V.V., Poedts, S., Lecacheux, A.: Solar Decameter Spikes. Solar Physics289(5), 1701–1714 (2014) https://doi.org/10.1007/s11207-013-0434-1

    work page doi:10.1007/s11207-013-0434-1 2014

  17. [17]

    Solar Physics291(1), 211–228 (2016) https://doi.org/10.1007/ s11207-015-0799-4

    Shevchuk, N.V., Melnik, V.N., Poedts, S., Dorovskyy, V.V., Magdalenic, J., Konovalenko, A.A., Brazhenko, A.I., Briand, C., Frantsuzenko, A.V., Rucker, H.O., Zarka, P.: The Storm of Decameter Spikes During the Event of 14 June 2012. Solar Physics291(1), 211–228 (2016) https://doi.org/10.1007/ s11207-015-0799-4

    work page 2012

  18. [18]

    The Astrophysical Journal 946(1), 33 (2023) https://doi.org/10.3847/1538-4357/acbd3f arXiv:2302.11265 [astro-ph.SR]

    Clarkson, D.L., Kontar, E.P., Vilmer, N., Gordovskyy, M., Chen, X., Chrysaphi, N.: Solar Radio Spikes and Type IIIb Striae Manifestations of Subsecond Electron Acceleration Triggered by a Coronal Mass Ejection. The Astrophysical Journal 946(1), 33 (2023) https://doi.org/10.3847/1538-4357/acbd3f arXiv:2302.11265 [astro-ph.SR]

    work page doi:10.3847/1538-4357/acbd3f 2023

  19. [19]

    The Astrophysical Journal917(2), 32 (2021) https://doi.org/10.3847/ 2041-8213/ac1a7d arXiv:2108.06191 [astro-ph.SR]

    Clarkson, D.L., Kontar, E.P., Gordovskyy, M., Chrysaphi, N., Vilmer, N.: First Frequency-time-resolved Imaging Spectroscopy Observations of Solar Radio Spikes. The Astrophysical Journal917(2), 32 (2021) https://doi.org/10.3847/ 2041-8213/ac1a7d arXiv:2108.06191 [astro-ph.SR]

    work page arXiv 2021

  20. [20]

    Australian Journal of Physics11, 215 (1958) https://doi.org/10.1071/PH580215

    Roberts, J.A.: Evidence of Echoes in the Solar Corona from a New Type of Burst. Australian Journal of Physics11, 215 (1958) https://doi.org/10.1071/PH580215

    work page doi:10.1071/ph580215 1958

  21. [21]

    Australian Journal of Physics22, 177 (1969) https://doi.org/10.1071/PH690177

    Ellis, G.R.A.: Fine structure in the spectra of solar radio bursts. Australian Journal of Physics22, 177 (1969) https://doi.org/10.1071/PH690177

    work page doi:10.1071/ph690177 1969

  22. [22]

    Astronomy & astrophysics12, 371 (1971)

    de La Noe, J., Moller Pedersen, B.: Relationship between Drift Pair Bursts and Decametre Type III Solar Radio Emission. Astronomy & astrophysics12, 371 (1971)

    work page 1971

  23. [23]

    drifting pairs

    Abranin, E.P., Bazelian, L.L., Goncharov, N.I., Zaitsev, V.V., Zinichev, V.A., Levin, B.N., Rapoport, V.O., Tsybko, I.G.: Some results of observations of solar radio bursts of the “drifting pairs” type near frequencies of 25 and 12.5 MHz. Astronomicheskii Zhurnal54, 146 (1977)

    work page 1977

  24. [24]

    Solar Physics231(1-2), 143–155 (2005) https://doi.org/10.1007/ s11207-005-8272-4

    Melnik, V.N., Konovalenko, A.A., Dorovskyy, V.V., Rucker, H.O., Abranin, E.P., Lisachenko, V.N., Lecacheux, A.: Solar Drift Pair Bursts in the Decame- ter Range. Solar Physics231(1-2), 143–155 (2005) https://doi.org/10.1007/ s11207-005-8272-4

    work page 2005

  25. [25]

    Astronomy & astrophysics631, 7 (2019) https://doi.org/10

    Kuznetsov, A.A., Kontar, E.P.: First imaging spectroscopy observations of solar drift pair bursts. Astronomy & astrophysics631, 7 (2019) https://doi.org/10. 1051/0004-6361/201936447 arXiv:1910.09864 [astro-ph.SR] 27

    work page arXiv 2019

  26. [26]

    The Astro- physical Journal898(2), 94 (2020) https://doi.org/10.3847/1538-4357/aba04a arXiv:2007.14648 [astro-ph.SR]

    Kuznetsov, A.A., Chrysaphi, N., Kontar, E.P., Motorina, G.: Radio Echo in the Turbulent Corona and Simulations of Solar Drift-pair Radio Bursts. The Astro- physical Journal898(2), 94 (2020) https://doi.org/10.3847/1538-4357/aba04a arXiv:2007.14648 [astro-ph.SR]

    work page doi:10.3847/1538-4357/aba04a 2020

  27. [27]

    The Astro- physical Journal956(2), 112 (2023) https://doi.org/10.3847/1538-4357/acf6c1 arXiv:2308.05839 [astro-ph.SR]

    Kontar, E.P., Emslie, A.G., Clarkson, D.L., Chen, X., Chrysaphi, N., Azzollini, F., Jeffrey, N.L.S., Gordovskyy, M.: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations. The Astro- physical Journal956(2), 112 (2023) https://doi.org/10.3847/1538-4357/acf6c1 arXiv:2308.05839 [astro-ph.SR]

    work page doi:10.3847/1538-4357/acf6c1 2023

  28. [28]

    The Astrophysical Journal 857(2), 82 (2018) https://doi.org/10.3847/1538-4357/aab60f

    Krupar, V., Maksimovic, M., Kontar, E.P., Zaslavsky, A., Santolik, O., Soucek, J., Kruparova, O., Eastwood, J.P., Szabo, A.: Interplanetary Type III Bursts and Electron Density Fluctuations in the Solar Wind. The Astrophysical Journal 857(2), 82 (2018) https://doi.org/10.3847/1538-4357/aab60f

    work page doi:10.3847/1538-4357/aab60f 2018

  29. [29]

    Monthly Notices of the Royal Astronomical Society520(2), 3117–3126 (2023) https://doi.org/10.1093/mnras/stad325 arXiv:2301.11299 [astro-ph.SR]

    Chen, X., Kontar, E.P., Clarkson, D.L., Chrysaphi, N.: The frequency ratio and time delay of solar radio emissions with fundamental and harmonic components. Monthly Notices of the Royal Astronomical Society520(2), 3117–3126 (2023) https://doi.org/10.1093/mnras/stad325 arXiv:2301.11299 [astro-ph.SR]

    work page doi:10.1093/mnras/stad325 2023

  30. [31]

    The Astrophysi- cal Journal Letters991(2), 57 (2025) https://doi.org/10.3847/2041-8213/ae09b0 arXiv:2509.17861 [astro-ph.SR]

    Kontar, E.P., Emslie, A.G., Clarkson, D.L., Pitňa, A.: Ion-scale Turbulence and Energy Cascade Rate in the Solar Corona and Inner Heliosphere. The Astrophysi- cal Journal Letters991(2), 57 (2025) https://doi.org/10.3847/2041-8213/ae09b0 arXiv:2509.17861 [astro-ph.SR]

    work page doi:10.3847/2041-8213/ae09b0 2025

  31. [32]

    Testing the ΛCDM Cosmological Model with Forthcoming Mea- surements of the Cosmic Microwave Background with SPT-3G

    Pitňa, A., Šafránková, J., Němeček, Z., Franci, L., Pi, G., Montagud Camps, V.: Characteristics of Solar Wind Fluctuations at and below Ion Scales. The Astrophysical Journal879(2), 82 (2019) https://doi.org/10.3847/1538-4357/ ab22b8

    work page doi:10.3847/1538-4357/ 2019

  32. [33]

    Journal of Geophys- ical Research (Space Physics)111(A4), 04102 (2006) https://doi.org/10.1029/ 2005JA011416

    Coles, W.A., Harmon, J.K., Sulzer, M.P., Chau, J.L., Woodman, R.F.: An upper bound on the solar radar cross section at 50 MHz. Journal of Geophys- ical Research (Space Physics)111(A4), 04102 (2006) https://doi.org/10.1029/ 2005JA011416

    work page 2006

  33. [34]

    LOFAR: The LOw-Frequency ARray

    van Haarlem, M.P., Wise, M.W., Gunst, A.W., Heald, G., McKean, J.P., Hes- sels, J.W.T., de Bruyn, A.G., Nijboer, R., Swinbank, J., Fallows, R., Brentjens, M., Nelles, A., Beck, R., Falcke, H., Fender, R., Hörandel, J., Koopmans, L.V.E., Mann, G., Miley, G., Röttgering, H., Stappers, B.W., Wijers, R.A.M.J., Zaroubi, S., van den Akker, M., Alexov, A., Ander...

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220873 2013

  34. [35]

    Solar Physics275(1-2), 17–40 (2012) https://doi.org/10.1007/ s11207-011-9776-8 29

    Lemen, J.R., Title, A.M., Akin, D.J., Boerner, P.F., Chou, C., Drake, J.F., Dun- can, D.W., Edwards, C.G., Friedlaender, F.M., Heyman, G.F., Hurlburt, N.E., Katz, N.L., Kushner, G.D., Levay, M., Lindgren, R.W., Mathur, D.P., McFeaters, E.L., Mitchell, S., Rehse, R.A., Schrijver, C.J., Springer, L.A., Stern, R.A., Tar- bell, T.D., Wuelser, J.-P., Wolfson, ...

    work page 2012

  35. [36]

    Solar Physics275(1-2), 3–15 (2012) https://doi.org/10.1007/ s11207-011-9841-3

    Pesnell, W.D., Thompson, B.J., Chamberlin, P.C.: The Solar Dynamics Obser- vatory (SDO). Solar Physics275(1-2), 3–15 (2012) https://doi.org/10.1007/ s11207-011-9841-3

    work page 2012

  36. [37]

    Solar Physics275(1-2), 229–259 (2012) https://doi.org/10

    Schou, J., Scherrer, P.H., Bush, R.I., Wachter, R., Couvidat, S., Rabello-Soares, M.C., Bogart, R.S., Hoeksema, J.T., Liu, Y., Duvall, T.L., Akin, D.J., Allard, B.A., Miles, J.W., Rairden, R., Shine, R.A., Tarbell, T.D., Title, A.M., Wolfson, C.J., Elmore, D.F., Norton, A.A., Tomczyk, S.: Design and Ground Calibration of the Helioseismic and Magnetic Imag...

    work page 2012

  37. [38]

    Solar Physics6(3), 442–455 (1969) https://doi.org/10.1007/ BF00146478

    Schatten, K.H., Wilcox, J.M., Ness, N.F.: A model of interplanetary and coro- nal magnetic fields. Solar Physics6(3), 442–455 (1969) https://doi.org/10.1007/ BF00146478

    work page 1969

  38. [39]

    Solar Physics , author =

    Altschuler, M.D., Newkirk, G. Jr.: Magnetic Fields and the Structure of the Solar Corona. I: Methods of Calculating Coronal Fields. Solar Physics9(1), 131–149 (1969) https://doi.org/10.1007/BF00145734

    work page doi:10.1007/bf00145734 1969

  39. [40]

    Solar type III radio burst time characteristics at LOFAR frequencies and the implications for electron beam transport

    Reid, H.A.S., Kontar, E.P.: Solar type III radio burst time characteristics at LOFAR frequencies and the implications for electron beam transport. Astronomy & Astrophysics614, 69 (2018) https://doi.org/10.1051/0004-6361/201732298 arXiv:1802.01507 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201732298 2018

  40. [41]

    , keywords =

    Condon, J.J.: Errors in elliptical gaussian fits. Publications of the Astronomical Society of the Pacific109(732), 166 (1997) https://doi.org/10.1086/133871

    work page doi:10.1086/133871 1997

  41. [42]

    The Astro- physical Journal925(2), 140 (2022) https://doi.org/10.3847/1538-4357/ac3bb7 arXiv:2111.07777 [astro-ph.SR]

    Gordovskyy, M., Kontar, E.P., Clarkson, D.L., Chrysaphi, N., Browning, P.K.: Sizes and Shapes of Sources in Solar Metric Radio Bursts. The Astro- physical Journal925(2), 140 (2022) https://doi.org/10.3847/1538-4357/ac3bb7 arXiv:2111.07777 [astro-ph.SR]

    work page doi:10.3847/1538-4357/ac3bb7 2022

  42. [43]

    Gordovskyy, M., Kontar, E., Browning, P., Kuznetsov, A.: Frequency–Distance StructureofSolarRadioSourcesObservedbyLOFAR.TheAstrophysicalJournal 873(2019) https://doi.org/10.3847/1538-4357/ab03d8

    work page doi:10.3847/1538-4357/ab03d8 2019

  43. [44]

    Solar Physics212(1), 165–200 (2003) https://doi.org/10.1023/A:1022908504100

    Schrijver, C.J., De Rosa, M.L.: Photospheric and heliospheric magnetic fields. Solar Physics212(1), 165–200 (2003) https://doi.org/10.1023/A:1022908504100

    work page doi:10.1023/a:1022908504100 2003

  44. [45]

    The Astrophysical Journal 899(1), 19 (2020) https://doi.org/10.3847/1538-4357/ab9cad arXiv:2006.08252 [astro-ph.SR]

    Chen, H., Zhang, J., De Pontieu, B., Ma, S., Kliem, B., Priest, E.: Coronal Mini- jets in an Activated Solar Tornado-like Prominence. The Astrophysical Journal 899(1), 19 (2020) https://doi.org/10.3847/1538-4357/ab9cad arXiv:2006.08252 [astro-ph.SR]

    work page doi:10.3847/1538-4357/ab9cad 2020

  45. [46]

    Astronomy & astrophysics683, 56 (2024) https://doi.org/10

    Gerekos, C., Steinbrügge, G., Jebaraj, I.C., Casillas, A., Donini, E., Sánchez- Cano, B., Lester, M.,Magdalenić, J., Peters, S.T., Romero-Wolf,A., Blankenship, 30 D.D.: Observation of solar radio burst events from Mars orbit with the Shallow Radar instrument. Astronomy & astrophysics683, 56 (2024) https://doi.org/10. 1051/0004-6361/202347900 arXiv:2307.01...

    work page arXiv 2024

  46. [47]

    Total” – full bursts spanning 38–60 MHz; “Image

    Ma, S., Kontar, E., Clarkson, D., Chen, H., Yan, Y.: Radio_waves: Radio Wave Transport in Solar Wind Including Anisotropic Scattering. https://doi.org/10. 5281/zenodo.19688827 . Fixed version for Ma et al. 2026 (Nature Communica- tions) Acknowledgements This paper is based (in part) on data obtained with the LOFAR telescope (LOFAR- ERIC) under project cod...

    work page 2026