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REVIEW 2 major objections 4 minor 1 cited by

An assessment of observational coverage and gaps for robust Sun to heliosphere integrated science

T0 review · 2 major / 4 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read The paper argues that solar-wind science can track density and speed end to end, but temperature, magnetic field, and non-thermal diagnostics stop below about two solar radii, leaving a large observational gap.

desk verdict Useful community assessment of observational coverage, but Section 4 overstates the temperature gap by ignoring the paper's own CODEX 3–8 R_sun description. read the letter →

arxiv 2502.06036 v3 pith:Q7WNI3G5 submitted 2025-02-09 astro-ph.SR physics.plasm-phphysics.space-ph

Yeimy J. Rivera , Samuel T. Badman This is my paper · ORCID
classification astro-ph.SRphysics.plasm-phphysics.space-ph
keywords solarwindcoronaheliosphereobservationalcoveragefieldsofviewinsitudiagnosticsremotesensingspacecraftcoordination
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This review asks whether the community can trace a single parcel of solar wind continuously from its birth in the corona to its interception by an inner-heliospheric spacecraft. The authors map the fields of view of current and near-future observatories against the in-situ trajectories of the two inner-heliospheric probes and find a sharp asymmetry: density and outflow speed can be tracked almost seamlessly from the low corona far into the heliosphere, whereas temperature, magnetic field, and non-thermal diagnostics exist only below about $2\,R_\odot$. That asymmetry means end-to-end thermodynamic and magnetic studies of the same plasma are not yet possible, even though radial-flow studies are. The paper therefore gives the community a concrete target for the next generation of instruments and observing campaigns.

What carries the argument

The central object is a coverage map: for each plasma diagnostic (electron and ion density, ion and electron temperature, outflow velocity, magnetic field, and non-thermal line broadening), the paper stacks the radial fields of view of all relevant instruments and marks where in-situ sampling begins. The map only counts an observation as usable for connection science when the remote view and the in-situ stream line up in quadrature, so that a spacecraft crosses plasma whose emission was imaged near the limb. The machinery's work is to make visible, in one picture, which physical quantities have continuous Sun-to-heliosphere coverage and which break off at the boundary of the low corona.

What would settle it

A concrete check would be to run a coordinated quadrature campaign once the new wide-field and ISS coronagraphs are in operation and ask whether electron temperature and magnetic field can actually be measured along one flux tube from $1.5\,R_\odot$ to the first in-situ crossing; if an unambiguous temperature or magnetic-field profile across $3$-$8\,R_\odot$ is obtained and matches the in-situ values, the claimed gap for those two quantities would be closed. The same campaign would falsify the gap if it showed that non-thermal line broadening can be measured above $2\,R_\odot$ with existing spectropolarimeters rather than only at the limb.

Watch

Extended reading notes

Core claim

The paper's central assessment is that, when observing geometry cooperates, density and velocity diagnostics now bridge the low corona to the inner heliosphere, but the plasma state variables that control solar-wind energetics do not. Temperature, magnetic field, and non-thermal information are effectively confined to the low corona, below $2\,R_\odot$, leaving a large observational gap between those remote measurements and their in-situ counterparts in the young solar wind. The authors reach this by overlaying each instrument's radial field of view with the orbits of the near-Sun spacecraft and by requiring a quadrature geometry, in which a spacecraft crosses plasma that has just been imaged at the solar limb. They argue that closing the gap requires off-limb spectroscopy of the extended corona and closer in-situ magnetic-field sampling, and that coordinated studies, while increasingly routine, still depend on rare line-ups of spacecraft and on overlapping operational windows.

Load-bearing premise

The whole coverage map assumes the planned missions, especially the wide-field imager, the ISS coronagraph, and the Phase-A EUV spectrograph, actually launch, operate, and perform as scheduled; if any of them slips, is descoped, or underperforms, the good density and velocity coverage (and the bad temperature and magnetic-field coverage) would both shift.

Editorial extensions

If this is right

  • Density and velocity profiles of individual solar-wind streams can become a standard product: with the new wide-field imagers and coronagraphs, a single stream can be followed from the low corona to well beyond $30\,R_\odot$ and matched to in-situ data.
  • Without extended-corona temperature diagnostics, claims about non-adiabatic heating and acceleration of the solar wind cannot be checked against observations in the region where most of that heating occurs.
  • The missing middle-corona magnetic-field and non-thermal measurements leave wave-energy flux and turbulence models underconstrained, so models of Alfvénic driving of the fast wind will remain fitted rather than tested.
  • Coordinated connection studies will stay rare and event-limited; the quadrature requirement plus overlapping operational windows means full end-to-end coverage is possible only in short windows.
  • The paper's priority list for future instrumentation—off-limb spectroscopy in the extended corona and closer in-situ magnetic-field sampling—follows directly from the gap, not from any single mission's science goals.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • An editor's inference: the coverage map implies that the highest-value new observations are not additional white-light imagers but spectropolarimetric capabilities above $2\,R_\odot$; those would turn the demonstrated density and velocity connectivity into thermal and magnetic connectivity.
  • One testable extension of the paper's argument would be to use young-wind in-situ measurements of temperature and magnetic field, plus a smooth-expansion assumption, to backward-reconstruct the middle-corona values and compare them with low-corona observations; disagreement would reveal where the gap actually bites.
  • The quadrature framework also suggests a metric for mission planning: the number of hours per year in which at least one remote observatory and one in-situ probe can observe the same flux tube, which could be computed from current ephemerides and used to rank candidate orbits.
  • Finally, the gap may be partially filled without new missions by exploiting total solar eclipses, which provide off-limb spectroscopy up to a few solar radii; the paper notes this but leaves it out of the coverage figures because eclipses are rare and short.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. This proceedings paper surveys remote and in situ instrumentation relevant to Sun-to-heliosphere connectivity science. It catalogs density, temperature, velocity, magnetic-field, and non-thermal diagnostics from active, near-future, and planned missions (Parker Solar Probe, Solar Orbiter, SOHO/STEREO, MLSO, Proba-3, Aditya-L1/VELC, CODEX, PUNCH, COSMO, ECCCO), displays radial coverage in Figures 1–5, reviews several recent coordinated studies, and concludes that density and velocity coverage can be excellent when coupled, while temperature, magnetic-field, and non-thermal diagnostics are largely confined to the low corona below 2 R_sun. The paper closes with a recommendation for new extended-corona spectroscopy and polarimetry.

Significance. The paper is a useful, concise community assessment rather than a new quantitative result. Its value lies in the organized inventory of overlapping fields of view and diagnostics, the explicit separation of remote-sensing limitations (line-of-sight integration, inversion) from in situ single-point limitations, and the review of recent coordinated campaigns. It also makes a specific, actionable claim about where coverage gaps remain, which can inform mission prioritization and observation planning. The main caveat is that the assessment is qualitative and time-dependent, and one of its summary statements is internally inconsistent with the instrument descriptions given earlier.

major comments (2)
  1. [§4, cf. §2.2.6 and §2.5] The summary sentence "temperature, magnetic field and non-thermal diagnostics are much more limited to the low corona, below 2R_sun" is not consistent with the instrument descriptions earlier in the paper. Section 2.2.6 states that CODEX provides electron density, temperature, and radial speed "between 3-8R_sun," and Section 2.5 explicitly identifies CODEX as "the only active mission ... that provides electron temperature from 3-8R_sun," while noting its ISS-related duty-cycle and lifetime limits (a few months). The summary therefore overstates the temperature gap by lumping temperature with magnetic-field and non-thermal diagnostics, which are indeed concentrated below 2 R_sun. Because the paper's actionable conclusion is that extended-corona temperature measurements should be prioritized, the summary should be reworded to say that, apart from CODEX's short-lived 3–8 R_sun electron-temperature channel and planned instruments such as ECCCO and COSMO, temperature coverage in the extended corona is essentially absent. As written, the central claim could misdirect priorities toward new temperature measurements rather than toward sustaining/validating CODEX and addressing the magnetic-field and non-thermal gaps.
  2. [§4, cf. §1 and §3] The statement that integrating remote and in situ measurements is "limited to when the remote observations are taken in quadrature with in situ observations" is too strong for the methods the paper itself discusses. Section 1 describes ballistic/PFSS mapping and MHD tracing as established ways to connect in situ streams to coronal sources without requiring quadrature, and Section 3 frames quadrature as "the optimal configuration" for tracking radial outflows rather than as a strict requirement. The final wording should be softened to "most directly achieved" or "best enabled by" quadrature alignment, with non-quadrature connection methods acknowledged, so that the assessment of coordination opportunities is not overstated.
minor comments (4)
  1. [§1] There is a typo in the Introduction: "heliopsphysics" should be "heliophysics."
  2. [Abstract] The Keywords field is empty; either populate it with relevant terms or remove the placeholder.
  3. [§2.5] The sentence "With the inclusion of CODEX and PUNCH, there will be several instruments that could provide velocity diagnostics as close to the Sun as 1.7R_sun" is slightly confusing because Metis is already an active instrument; consider rewording to "With CODEX and PUNCH joining existing instruments such as Metis...".
  4. [§2.3.3] The Phase A status of ECCCO is time-sensitive; adding "as of this writing" would make the assessment less perishable.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: this is an instrument-coverage assessment based on mission documentation, not a derivation from fitted parameters or self-cited results.

full rationale

The paper is a survey and assessment of observational coverage and gaps for Sun-to-heliosphere science. Its central claims are about which plasma diagnostics are available in which radial ranges, supported by descriptions of mission instruments, fields of view, and operational status drawn from external mission documentation. There is no derivation chain, no fitted parameter renamed as a prediction, and no uniqueness theorem imported from prior work. The authors cite their own related studies (e.g., Rivera et al. 2024b, Rivera et al. 2025) as examples of coordinated observational studies, but those citations are illustrative rather than load-bearing for the coverage conclusions; the coverage maps and gap assessments stand on instrument specifications, not on the authors' prior results. The possible tension between Section 2.2.6, which states that CODEX provides electron temperature between 3 and 8 R_sun, and Section 4, which states that temperature diagnostics are 'much more limited to the low corona, below 2R_sun,' is an internal consistency or accuracy concern, not a circularity concern, because the conclusion does not reduce to its own inputs by definition. Accordingly, no circular steps are identified and the circularity score is 0.

Assumptions & free parameters 0 free parameters · 3 assumptions · 0 invented entities

The paper contributes a synthesis, not a model. It introduces no free parameters or invented entities. Its conclusions rest on domain assumptions about instrument specifications and the geometry required for connection studies, all drawn from the cited mission literature.

assumptions (3)
  • domain assumption The instrument FOVs and diagnostics listed in Section 2 are accurate as reported by mission teams.
    Figures 1-5 are built from these values; the paper does not independently calibrate them.
  • domain assumption Quadrature geometry between remote and in situ observers is necessary for meaningful Sun-to-heliosphere connection science.
    Section 3 states the optimal configuration requires spacecraft to intercept wind whose source is near the observed limb.
  • domain assumption Steady-state mapping techniques are adequate for source identification except for transients.
    Section 1 discusses the limitation but the paper's examples rely on these mappings.

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Cite this review

Pith. "Pith review of An assessment of observational coverage and gaps for robust Sun to heliosphere integrated science." pith.science (2026). https://pith.science/paper/Q7WNI3G5

@misc{pith2026250206036,
  author       = {Pith},
  title        = {Pith review of: An assessment of observational coverage and gaps for robust Sun to heliosphere integrated science},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/Q7WNI3G5}},
  note         = {Machine review of arXiv:2502.06036}
}
read the original abstract

Understanding the generation and development of the continuous outflow from the Sun requires tracing the physical conditions from deep in the corona to the heliosphere. Detailed global observations of plasma state variables and the magnetic field are needed to provide critical constraints to the underlying physics driving models of the corona and solar wind. Key diagnostics of the solar wind require measurements at its formation site and during its outflow to continuously track it across rapidly changing regions of space. A unified view of the solar wind is only possible through coordinated remote and in situ observations that probe these different regions. Here, we discuss current observational coverage and gaps of different plasma properties and review recent coordinated studies. We highlight how these efforts may become more routine with the launch of upcoming and planned missions.

Figures

Figures reproduced from arXiv: 2502.06036 by the authors.

Figure 1
Figure 1. The image contains the field of view (FOV) of different ground and space-based instruments for density diagnostics of the low to outer corona described in Section 2.1. Although we only use a small wedge to illustrate radial coverage, all instruments take remote observations of the full corona. We also include in situ coverage from Parker that ranges ±4 ◦ from the ecliptic plane. The background image is a composite o… view at source ↗
Figure 2
Figure 2. The image shows a zoomed out version of [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Same as [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p008_5.png]

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    astro-ph.SR 2025-08 conditional novelty 7.0 of 10

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Reference graph

Works this paper leans on

104 extracted references · 25 canonical work pages · cited by 1 Pith paper

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry add.period write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTIO...

  2. [2]

    K., et al

    Abbo , L., Ofman , L., Antiochos , S. K., et al. 2016, Space Science Reviews, 201, 55, 10.1007/s11214-016-0264-1

    doi:10.1007/s11214-016-0264-1 2016

  3. [3]

    P., Telloni , D., & Zhao , L

    Adhikari , L., Zank , G. P., Telloni , D., & Zhao , L. L. 2022, The Astrophysical Journal Letters, 937, L29, 10.3847/2041-8213/ac91c6

    doi:10.3847/2041-8213/ac91c6 2022

  4. [4]

    K., Miki \'c , Z., Titov , V

    Antiochos , S. K., Miki \'c , Z., Titov , V. S., Lionello , R., & Linker , J. A. 2011, The Astrophysical Journal, 731, 112, 10.1088/0004-637X/731/2/112

    doi:10.1088/0004-637x/731/2/112 2011

  5. [5]

    T., Bale , S

    Badman , S. T., Bale , S. D., Mart \' nez Oliveros , J. C., et al. 2020, The Astrophysical Journal Supplement, 246, 23, 10.3847/1538-4365/ab4da7

    doi:10.3847/1538-4365/ab4da7 2020

  6. [6]

    T., Riley , P., Jones , S

    Badman , S. T., Riley , P., Jones , S. I., et al. 2023, Journal of Geophysical Research (Space Physics), 128, e2023JA031359, 10.1029/2023JA031359

    doi:10.1029/2023ja031359 2023

  7. [7]

    L., et al

    Baker , D., D \'e moulin , P., Yardley , S. L., et al. 2023, The Astrophysical Journal, 950, 65, 10.3847/1538-4357/acc653

    doi:10.3847/1538-4357/acc653 2023

  8. [8]

    D., Goetz , K., Harvey , P

    Bale , S. D., Goetz , K., Harvey , P. R., et al. 2016, Space Science Reviews, 204, 49, 10.1007/s11214-016-0244-5

    doi:10.1007/s11214-016-0244-5 2016

Show all 104 references
  1. [9]

    D., Drake , J

    Bale , S. D., Drake , J. F., McManus , M. D., et al. 2023, Nature, 618, 252, 10.1038/s41586-023-05955-3

    2023 doi

  2. [10]

    2018, The Astrophysical Journal, 859, 155, 10.3847/1538-4357/aabfb7

    Boe , B., Habbal , S., Druckm \"u ller , M., et al. 2018, The Astrophysical Journal, 859, 155, 10.3847/1538-4357/aabfb7

    2018 doi

  3. [11]

    H., Ugarte-Urra , I., & Warren , H

    Brooks , D. H., Ugarte-Urra , I., & Warren , H. P. 2015, Nature Communications, 6, 5947, 10.1038/ncomms6947

    2015 doi

  4. [12]

    H., Warren , H

    Brooks , D. H., Warren , H. P., Baker , D., Matthews , S. A., & Yardley , S. L. 2024, The Astrophysical Journal, 976, 188, 10.3847/1538-4357/ad87ef

    2024 doi

  5. [13]

    H., Winebarger , A

    Brooks , D. H., Winebarger , A. R., Savage , S., et al. 2020, The Astrophysical Journal, 894, 144, 10.3847/1538-4357/ab8a4c

    2020 doi

  6. [14]

    H., Janvier , M., Baker , D., et al

    Brooks , D. H., Janvier , M., Baker , D., et al. 2022, The Astrophysical Journal, 940, 66, 10.3847/1538-4357/ac9b0b

    2022 doi

  7. [15]

    E., Howard , R

    Brueckner , G. E., Howard , R. A., Koomen , M. J., et al. 1995, Solar Physics, 162, 357, 10.1007/BF00733434

    1995 doi

  8. [16]

    2013, Living Reviews in Solar Physics, 10, 2, 10.12942/lrsp-2013-2

    Bruno , R., & Carbone , V. 2013, Living Reviews in Solar Physics, 10, 2, 10.12942/lrsp-2013-2

    2013 doi

  9. [17]

    S., Kim , Y.-H., et al

    Casti , M., Newmark , J. S., Kim , Y.-H., et al. 2024, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 13092, Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave, ed. L. E. Coyle , S. Matsuura , & M. D. Perrin ...

    2024 doi

  10. [18]

    P., Seaton , D

    Chitta , L. P., Seaton , D. B., Downs , C., DeForest , C. E., & Higginson , A. K. 2023 a , Nature Astronomy, 7, 133, 10.1038/s41550-022-01834-5

    2023 doi

  11. [19]

    P., Zhukov , A

    Chitta , L. P., Zhukov , A. N., Berghmans , D., et al. 2023 b , Science, 381, 867, 10.1126/science.ade5801

    2023 doi

  12. [20]

    Dakeyo , J.-B., Maksimovic , M., D \'e moulin , P., Halekas , J., & Stevens , M. L. 2022, The Astrophysical Journal, 940, 130, 10.3847/1538-4357/ac9b14

    2022 doi

  13. [21]

    T., et al

    de Pablos , D., Samanta , T., Badman , S. T., et al. 2022, Solar Physics, 297, 90, 10.1007/s11207-022-02022-4

    2022 doi

  14. [22]

    G., Burkepile , J

    de Wijn , A. G., Burkepile , J. T., Tomczyk , S., et al. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 8444, Ground-based and Airborne Telescopes IV, ed. L. M. Stepp , R. Gilmozzi , & H. J. Hall , 84443N, 10.1117/12.926511

    2012 doi

  15. [23]

    2022, in 2022 IEEE Aerospace Conference (AERO), 1--11, 10.1109/AERO53065.2022.9843340

    DeForest, C., Killough, R., Gibson, S., et al. 2022, in 2022 IEEE Aerospace Conference (AERO), 1--11, 10.1109/AERO53065.2022.9843340

    2022

  16. [24]

    2023, The Astrophysical Journal Supplement, 265, 11, 10.3847/1538-4365/acad68

    Del Zanna , G., Samra , J., Monaghan , A., et al. 2023, The Astrophysical Journal Supplement, 265, 11, 10.3847/1538-4365/acad68

    2023 doi

  17. [25]

    Domingo , V., Fleck , B., & Poland , A. I. 1995, Solar Physics, 162, 1, 10.1007/BF00733425

    1995 doi

  18. [26]

    D., Badman, S

    Ervin, T., Bale, S. D., Badman, S. T., et al. 2024, The Astrophysical Journal, 969, 83, 10.3847/1538-4357/ad4604

    2024 doi

  19. [27]

    J., Velli , M

    Fox , N. J., Velli , M. C., Bale , S. D., et al. 2016, Space Science Reviews, 204, 7, 10.1007/s11214-015-0211-6

    2016 doi

  20. [28]

    A., & Janzen , P

    Frazin , R. A., & Janzen , P. 2002, The Astrophysical Journal, 570, 408, 10.1086/339572

    2002 doi

  21. [29]

    A., V \'a squez , A

    Frazin , R. A., V \'a squez , A. M., Kamalabadi , F., & Park , H. 2007, The Astrophysical Journal Letters, 671, L201, 10.1086/525017

    2007 doi

  22. [30]

    E., Dalmasse , K., Rachmeler , L

    Gibson , S. E., Dalmasse , K., Rachmeler , L. A., et al. 2017, The Astrophysical Journal Letters, 840, L13, 10.3847/2041-8213/aa6fac

    2017 doi

  23. [31]

    S., Kim , Y.-H., et al

    Gong , Q., Newmark , J. S., Kim , Y.-H., et al. 2024, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 13092, Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave, ed. L. E. Coyle , S. Matsuura , & M. D. Perrin ,...

    2024 doi

  24. [32]

    R., Druckm \"u ller , M., Morgan , H., et al

    Habbal , S. R., Druckm \"u ller , M., Morgan , H., et al. 2010, The Astrophysical Journal, 708, 1650, 10.1088/0004-637X/708/2/1650

    2010 doi

  25. [33]

    2011, The Astrophysical Journal, 734, 120, 10.1088/0004-637X/734/2/120

    ---. 2011, The Astrophysical Journal, 734, 120, 10.1088/0004-637X/734/2/120

    2011 doi

  26. [34]

    R., Druckm \"u ller , M., Alzate , N., et al

    Habbal , S. R., Druckm \"u ller , M., Alzate , N., et al. 2021, The Astrophysical Journal Letters, 911, L4, 10.3847/2041-8213/abe775

    2021 doi

  27. [35]

    Hahn , M., & Savin , D. W. 2014, The Astrophysical Journal, 795, 111, 10.1088/0004-637X/795/2/111

    2014 doi

  28. [36]

    S., Whittlesey , P., Larson , D

    Halekas , J. S., Whittlesey , P., Larson , D. E., et al. 2022, The Astrophysical Journal, 936, 53, 10.3847/1538-4357/ac85b8

    2022 doi

  29. [37]

    S., Bale , S

    Halekas , J. S., Bale , S. D., Berthomier , M., et al. 2023, The Astrophysical Journal, 952, 26, 10.3847/1538-4357/acd769

    2023 doi

  30. [38]

    M., Gibson , S

    Hassler , D. M., Gibson , S. E., Newmark , J. S., et al. 2023, in Bulletin of the American Astronomical Society, Vol. 55, 164, 10.3847/25c2cfeb.408d006f

    2023 doi

  31. [39]

    M., & Marsch , E

    Hellinger , P., Matteini , L., S tver \'a k , S ., Tr \'a vn \' c ek , P. M., & Marsch , E. 2011, Journal of Geophysical Research (Space Physics), 116, A09105, 10.1029/2011JA016674

    2011 doi

  32. [40]

    S., O'Brien , H., Carrasco Blazquez , I., et al

    Horbury , T. S., O'Brien , H., Carrasco Blazquez , I., et al. 2020, Astronomy & Astrophysics, 642, A9, 10.1051/0004-6361/201937257

    2020 doi

  33. [41]

    A., Moses , J

    Howard , R. A., Moses , J. D., Vourlidas , A., et al. 2008, Space Science Reviews, 136, 67, 10.1007/s11214-008-9341-4

    2008 doi

  34. [42]

    V., Hick , P

    Jackson , B. V., Hick , P. P., Buffington , A., et al. 2011, Journal of Atmospheric and Solar-Terrestrial Physics, 73, 1214, 10.1016/j.jastp.2010.10.007

    2011 doi

  35. [43]

    C., Abiad , R., Austin , G., et al

    Kasper , J. C., Abiad , R., Austin , G., et al. 2016, Space Science Reviews, 204, 131, 10.1007/s11214-015-0206-3

    2016 doi

  36. [44]

    C., Klein , K

    Kasper , J. C., Klein , K. G., Lichko , E., et al. 2021, Physical Review Letters, 127, 255101, 10.1103/PhysRevLett.127.255101

    2021 doi

  37. [45]

    C., Zurbuchen , T

    Ko , Y.-K., Raymond , J. C., Zurbuchen , T. H., et al. 2006, The Astrophysical Journal, 646, 1275, 10.1086/505021

    2006 doi

  38. [46]

    L., Esser , R., Gardner , L

    Kohl , J. L., Esser , R., Gardner , L. D., et al. 1995, Solar Physics, 162, 313, 10.1007/BF00733433

    1995 doi

  39. [47]

    T., Dudok de Wit , T., et al

    Krasnoselskikh , V., Tsurutani , B. T., Dudok de Wit , T., et al. 2022, Experimental Astronomy, 54, 277, 10.1007/s10686-022-09878-1

    2022 doi

  40. [48]

    R., & Tomczyk , S

    Landi , E., Habbal , S. R., & Tomczyk , S. 2016, Journal of Geophysical Research (Space Physics), 121, 8237, 10.1002/2016JA022598

    2016 doi

  41. [49]

    2024, in EGU General Assembly Conference Abstracts, EGU General Assembly Conference Abstracts, 4200, 10.5194/egusphere-egu24-4200

    Linker , J., Downs , C., Caplan , R., et al. 2024, in EGU General Assembly Conference Abstracts, EGU General Assembly Conference Abstracts, 4200, 10.5194/egusphere-egu24-4200

    2024 doi

  42. [50]

    A., et al

    Lionello , R., Downs , C., Linker , J. A., et al. 2019, Solar Physics, 294, 13, 10.1007/s11207-019-1401-2

    2019 doi

  43. [51]

    I., et al

    Lionello , R., Downs , C., Mason , E. I., et al. 2023, The Astrophysical Journal, 959, 77, 10.3847/1538-4357/ad00be

    2023 doi

  44. [52]

    T., Raines , J

    Livi , S., Lepri , S. T., Raines , J. M., et al. 2023, Astronomy & Astrophysics, 676, A36, 10.1051/0004-6361/202346304

    2023 doi

  45. [53]

    G., V \'a squez , A

    Lloveras , D. G., V \'a squez , A. M., Landi , E., & Frazin , R. A. 2019, Boletin de la Asociacion Argentina de Astronomia La Plata Argentina, 61, 35

    2019

  46. [54]

    K., & Richter , K

    Marsch , E., Goertz , C. K., & Richter , K. 1982, Journal of Geophysical Research, 87, 5030, 10.1029/JA087iA07p05030

    1982 doi

  47. [55]

    I., Lionello , R., Downs , C., et al

    Mason , E. I., Lionello , R., Downs , C., et al. 2023, The Astrophysical Journal Letters, 959, L4, 10.3847/2041-8213/ad00bd

    2023 doi

  48. [56]

    J., Alexander , N., Angold , N., et al

    McComas , D. J., Alexander , N., Angold , N., et al. 2016, Space Science Reviews, 204, 187, 10.1007/s11214-014-0059-1

    2016 doi

  49. [57]

    U., et al

    Mishra , S., Sasikumar Raja , K., Sanal Krishnan , V. U., et al. 2024, Experimental Astronomy, 57, 7, 10.1007/s10686-024-09922-2

    2024 doi

  50. [58]

    J., Weberg , M

    Morton , R. J., Weberg , M. J., & McLaughlin , J. A. 2019, Nature Astronomy, 3, 223, 10.1038/s41550-018-0668-9

    2019 doi

  51. [59]

    M \"u ller , D., St. Cyr , O. C., Zouganelis , I., et al. 2020, Astronomy & Astrophysics, 642, A1, 10.1051/0004-6361/202038467

    2020 doi

  52. [60]

    2015, The Astrophysical Journal, 806, 55, 10.1088/0004-637X/806/1/55

    Oran , R., Landi , E., van der Holst , B., et al. 2015, The Astrophysical Journal, 806, 55, 10.1088/0004-637X/806/1/55

    2015 doi

  53. [61]

    J., Bruno , R., Livi , S., et al

    Owen , C. J., Bruno , R., Livi , S., et al. 2020, Astronomy & Astrophysics, 642, A16, 10.1051/0004-6361/201937259

    2020 doi

  54. [62]

    Y., et al

    Palmerio , E., Carcaboso , F., Khoo , L. Y., et al. 2024, The Astrophysical Journal, 963, 108, 10.3847/1538-4357/ad1ab4

    2024 doi

  55. [63]

    2024, The Astrophysical Journal Letters, 976, L6, 10.3847/2041-8213/ad8c45

    Ramesh , R., Muthu Priyal , V., Singh , J., et al. 2024, The Astrophysical Journal Letters, 976, L6, 10.3847/2041-8213/ad8c45

    2024 doi

  56. [64]

    E., Stenborg , G., Seaton , D

    Raouafi , N. E., Stenborg , G., Seaton , D. B., et al. 2023 a , The Astrophysical Journal, 945, 28, 10.3847/1538-4357/acaf6c

    2023 doi

  57. [65]

    E., Hoeksema , J

    Raouafi , N. E., Hoeksema , J. T., Newmark , J. S., et al. 2023 b , in Bulletin of the American Astronomical Society, Vol. 55, 333, 10.3847/25c2cfeb.c647a83d

    2023 doi

  58. [66]

    2023, in AAS/Solar Physics Division Meeting, Vol

    Reeves , K., Seaton , D., Cheimets , P., et al. 2023, in AAS/Solar Physics Division Meeting, Vol. 55, 54th Meeting of the Solar Physics Division, 302.06

    2023

  59. [67]

    2023, Solar Physics, 298, 73, 10.1007/s11207-023-02160-3

    Reginald , N., Newmark , J., & Rastaetter , L. 2023, Solar Physics, 298, 73, 10.1007/s11207-023-02160-3

    2023 doi

  60. [68]

    D., & Smith , C

    Richardson , J. D., & Smith , C. W. 2003, Geophysical Review letters, 30, 1206, 10.1029/2002GL016551

    2003 doi

  61. [69]

    A., et al

    Riley , P., Downs , C., Linker , J. A., et al. 2019, The Astrophysical Journal Letters, 874, L15, 10.3847/2041-8213/ab0ec3

    2019 doi

  62. [70]

    A., Miki \'c , Z., et al

    Riley , P., Linker , J. A., Miki \'c , Z., et al. 2006, The Astrophysical Journal, 653, 1510, 10.1086/508565

    2006 doi

  63. [71]

    Riley , P., Lionello , R., & Rivera , Y. J. 2025, The Astrophysical Journal, 979, 204, 10.3847/1538-4357/ada253

    2025 doi

  64. [72]

    R., Warner , M., Keil , S

    Rimmele , T. R., Warner , M., Keil , S. L., et al. 2020, Solar Physics, 295, 172, 10.1007/s11207-020-01736-7

    2020 doi

  65. [73]

    2024 a , in AGU Fall Meeting Abstracts, Vol

    Rivera , Y., Samra , J., Tritschler , A., et al. 2024 a , in AGU Fall Meeting Abstracts, Vol. 2024, SH53F--07

    2024

  66. [74]

    J., Higginson , A., Lepri , S

    Rivera , Y. J., Higginson , A., Lepri , S. T., et al. 2022, Frontiers in Astronomy and Space Sciences, 9, 417, 10.3389/fspas.2022.1056347

    2022

  67. [75]

    J., Badman , S

    Rivera , Y. J., Badman , S. T., Stevens , M. L., et al. 2024 b , Science, 385, 962, 10.1126/science.adk6953

    2024 doi

  68. [76]

    J., Badman , S

    Rivera , Y. J., Badman , S. T., Verniero , J. L., et al. 2025, The Astrophysical Journal, 980, 70, 10.3847/1538-4357/ada699

    2025 doi

  69. [77]

    2020, Astronomy & Astrophysics, 642, A8, 10.1051/0004-6361/201936663

    Rochus , P., Auch \`e re , F., Berghmans , D., et al. 2020, Astronomy & Astrophysics, 642, A8, 10.1051/0004-6361/201936663

    2020 doi

  70. [78]

    F., Mason , G

    Rodr \' guez-Pacheco , J., Wimmer-Schweingruber , R. F., Mason , G. M., et al. 2020, Astronomy & Astrophysics, 642, A7, 10.1051/0004-6361/201935287

    2020 doi

  71. [79]

    1997, in ESA Special Publication, Vol

    Romoli , M., Biesecker , D., Benna , C., et al. 1997, in ESA Special Publication, Vol. 404, Fifth SOHO Workshop: The Corona and Solar Wind Near Minimum Activity, ed. A. Wilson , 637

    1997

  72. [80]

    2021, Astronomy & Astrophysics, 656, A32, 10.1051/0004-6361/202140980

    Romoli , M., Antonucci , E., Andretta , V., et al. 2021, Astronomy & Astrophysics, 656, A32, 10.1051/0004-6361/202140980

    2021 doi

  73. [81]

    A., Petrie, G

    Schad, T. A., Petrie, G. J., Kuhn, J. R., et al. 2024, Science Advances, 10, eadq1604, 10.1126/sciadv.adq1604

    2024 doi

  74. [82]

    V., Zhukov , A

    Shestov , S. V., Zhukov , A. N., Inhester , B., Dolla , L., & Mierla , M. 2021, Astronomy & Astrophysics, 652, A4, 10.1051/0004-6361/202140467

    2021 doi

  75. [83]

    2020, Astronomy & Astrophysics, 642, A14, 10.1051/0004-6361/201935574

    SPICE Consortium , Anderson , M., Appourchaux , T., et al. 2020, Astronomy & Astrophysics, 642, A14, 10.1051/0004-6361/201935574

    2020 doi

  76. [84]

    C., Frandsen , A

    Stone , E. C., Frandsen , A. M., Mewaldt , R. A., et al. 1998, Space Science Reviews, 86, 1, 10.1023/A:1005082526237

    1998 doi

  77. [85]

    2022, The Astrophysical Journal, 926, 35, 10.3847/1538-4357/ac391810.1002/essoar.10508664.1

    Szente , J., Landi , E., & van der Holst , B. 2022, The Astrophysical Journal, 926, 35, 10.3847/1538-4357/ac391810.1002/essoar.10508664.1

    2022

  78. [86]

    2021, The Astrophysical Journal Letters, 920, L14, 10.3847/2041-8213/ac282f

    Telloni , D., Andretta , V., Antonucci , E., et al. 2021, The Astrophysical Journal Letters, 920, L14, 10.3847/2041-8213/ac282f

    2021 doi

  79. [87]

    P., et al

    Telloni , D., Adhikari , L., Zank , G. P., et al. 2022, The Astrophysical Journal Letters, 938, L8, 10.3847/2041-8213/ac9624

    2022 doi

  80. [88]

    2023, The Astrophysical Journal, 954, 108, 10.3847/1538-4357/aceb64

    Telloni , D., Romoli , M., Velli , M., et al. 2023, The Astrophysical Journal, 954, 108, 10.3847/1538-4357/aceb64

    2023 doi

  81. [89]

    V., Cota , L., et al

    Tiburzi , C., Jackson , B. V., Cota , L., et al. 2023, Advances in Space Research, 72, 5287, 10.1016/j.asr.2022.04.070

    2023 doi

  82. [90]

    W., Keil , S

    Tomczyk , S., McIntosh , S. W., Keil , S. L., et al. 2007, Science, 317, 1192, 10.1126/science.1143304

    2007 doi

  83. [91]

    L., Darnell , T., et al

    Tomczyk , S., Card , G. L., Darnell , T., et al. 2008, Solar Physics, 247, 411, 10.1007/s11207-007-9103-6

    2008 doi

  84. [92]

    T., et al

    Tomczyk , S., Landi , E., Burkepile , J. T., et al. 2016, Journal of Geophysical Research (Space Physics), 121, 7470, 10.1002/2016JA022871

    2016 doi

  85. [93]

    van de Hulst , H. C. 1950, Bulletin of the Astronomical Institutes of the Netherlands, 11, 135

    1950

  86. [94]

    B., Klein , K

    van der Holst , B., Manchester , IV, W. B., Klein , K. G., & Kasper , J. C. 2019, The Astrophysical Journal Letters, 872, L18, 10.3847/2041-8213/ab04a5

    2019 doi

  87. [95]

    M., Nuevo , F

    V \'a squez , A. M., Nuevo , F. A., Romoli , M., et al. 2024, Solar Physics, 299, 165, 10.1007/s11207-024-02410-y

    2024 doi

  88. [96]

    K., Vourlidas , A., et al

    Velli , M., Harra , L. K., Vourlidas , A., et al. 2020, Astronomy & Astrophysics, 642, A4, 10.1051/0004-6361/202038245

    2020 doi

  89. [97]

    2023, in Bulletin of the American Astronomical Society, Vol

    Viall , N., Desai , M., Attie , R., & Wallace , S. 2023, in Bulletin of the American Astronomical Society, Vol. 55, 417, 10.3847/25c2cfeb.87bd3c44

    2023 doi

  90. [98]

    M., & Borovsky , J

    Viall , N. M., & Borovsky , J. E. 2020, Journal of Geophysical Research (Space Physics), 125, e26005, 10.1029/2018JA02600510.1002/essoar.10502606.1

    2020

  91. [99]

    A., Fisk , L

    von Steiger , R., Schwadron , N. A., Fisk , L. A., et al. 2000, Journal of Geophysical Research, 105, 27217, 10.1029/1999JA000358

    2000 doi

  92. [100]

    L., Davila , J

    Wang , T., Reginald , N. L., Davila , J. M., St. Cyr , O. C., & Thompson , W. T. 2017, Solar Physics, 292, 97, 10.1007/s11207-017-1130-3

    2017 doi

  93. [101]

    J., Seaton , D

    West , M. J., Seaton , D. B., Wexler , D. B., et al. 2023, Solar Physics, 298, 78, 10.1007/s11207-023-02170-1

    2023 doi

  94. [102]

    B., Brosius , A

    Wilson , III, L. B., Brosius , A. L., Gopalswamy , N., et al. 2021, Reviews of Geophysics, 59, e2020RG000714, 10.1029/2020RG00071410.1002/essoar.10504309.2

    2021 arXiv

  95. [103]

    2024, Science, 386, 76, 10.1126/science.ado2993

    Yang, Z., Tian, H., Tomczyk, S., et al. 2024, Science, 386, 76, 10.1126/science.ado2993

    2024 doi

  96. [104]

    L., Brooks , D

    Yardley , S. L., Brooks , D. H., D'Amicis , R., et al. 2024, Nature Astronomy, 8, 953, 10.1038/s41550-024-02278-9

    2024 doi

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