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arxiv: 2606.24354 · v1 · pith:ODULMOY6new · submitted 2026-06-23 · 🌌 astro-ph.IM · astro-ph.SR

White paper on the relevance of the European Solar Telescope (EST) for the French heliophysics

E. Pariat , Q. Noraz , B. Perri , N. Poirier , C. Froment , L. Bigot , G. Aulanier , B. Gelly
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J. Aboudarham S. Aizawa O. Alexandrova S. Alqeeq T. Amari F. Auch\`ere G. Bernoux M. Berthomier V. Bommier X. Bonnin P. Boumier A. S. Brun I. Bual\'e E. Buchlin A. Canou P. Canu T. Corbard F. Cornu C. Coustillet G. Cozzani L. D'herbomez S. Diaz Castillo T. Dudok de Wit M. Faurobert A. Finley D. Fontaine R. A. Garcia R. Grappin L. Hadid K. H. Henadhira Arachchige M. Janvier L. Jouve R. Kieokaew H. Kirkwood B. Lavraud J.-P. Le Breton O. Le Contel N. Le Nestour F. Leblanc S. Masson N. Meyer-Vernet S. Parenti F. Pitout M. Rieutord J. Romero Casta\~neda A. Rouillard C. Ruiz de Galarreta F. Sahraoui B. Schmieder P. Simon A. Strugarek M. Tallon P. Thepthong J. Touresse J.-C. Vial N. Vilmer A. Zaslavsky
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Pith reviewed 2026-06-25 23:07 UTC · model grok-4.3

classification 🌌 astro-ph.IM astro-ph.SR
keywords European Solar Telescopeheliophysicsspace weathersolar photospheresolar chromosphereadaptive opticsFrench astrophysics
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The pith

The 4.2 m European Solar Telescope will supply French heliophysicists with high-resolution data on the solar photosphere and chromosphere for space weather studies.

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

The paper reviews how the European Solar Telescope, now in its crystallisation phase toward an ERIC, will deliver state-of-the-art observations of the Sun's lower atmosphere. It argues that the telescope's multi-conjugate adaptive optics, polarimetric and spectroscopic instruments will generate datasets particularly valuable to French solar physics and heliophysics groups. These observations are presented as essential for advancing understanding of dynamical events in the low solar atmosphere and for improving space weather applications.

Core claim

The EST will provide unprecedented observations of the solar photosphere and chromosphere and unrivaled datasets of high interest in the framework of space weather. It will advance numerous topics of solar physics as well as solar adaptive optics developments while supplying data sets relevant to French heliophysicists.

What carries the argument

The 4.2 m aperture telescope with multi-conjugate adaptive optics, light-polarisation analyser, imaging spectrograph and integral field unit spectrographs.

If this is right

  • Progress on French-priority topics in solar atmosphere dynamics and adaptive optics.
  • New high-resolution datasets for modeling solar events that affect Earth.
  • Support for space weather forecasting efforts using photospheric and chromospheric observations.
  • Strengthened French participation in European solar infrastructure projects.

Where Pith is reading between the lines

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

  • Securing access could position French teams to lead targeted programs on specific solar features.
  • The resulting data streams might be combined with existing French ground- and space-based assets for multi-instrument studies.
  • Long-term operation could shift European priorities toward sustained ground-based solar monitoring.

Load-bearing premise

The EST project will move beyond its crystallisation phase to full operation and French researchers will obtain access to its data.

What would settle it

Absence of an operational European Research Infrastructure Consortium or lack of formal data-access agreements for French institutions would prevent the described scientific benefits.

Figures

Figures reproduced from arXiv: 2606.24354 by A. Canou P. Canu, A. Finley, A. Rouillard, A. S. Brun, A. Strugarek, A. Zaslavsky, B. Gelly, B. Lavraud, B. Perri, B. Schmieder, C. Coustillet, C. Froment, C. Ruiz de Galarreta, D. Fontaine, E. Buchlin, E. Pariat, F. Auch\`ere, F. Cornu, F. LeBlanc, F. Pitout, F. Sahraoui, G. Aulanier, G. Bernoux, G. Cozzani, H. Kirkwood, I. Bual\'e, J. Aboudarham, J.-C. Vial, J.-P. Le Breton, J. Romero Casta\~neda, J. Touresse, K. H. Henadhira Arachchige, L. Bigot, L. D'herbomez, L. Hadid, L. Jouve, M. Berthomier, M. Faurobert, M. Janvier, M. Rieutord, M. Tallon, N. Le Nestour, N. Meyer-Vernet, N. Poirier, N. Vilmer, O. Alexandrova, O. Le Contel, P. Boumier, P. Simon, P. Thepthong, Q. Noraz, R. A. Garcia, R. Grappin, R. Kieokaew, S. Aizawa, S. Alqeeq, S. Diaz Castillo, S. Masson, S. Parenti, T. Amari, T. Corbard, T. Dudok de Wit, V. Bommier, X. Bonnin.

Figure 1
Figure 1. Figure 1: Example of solar granulation observed by THEMIS. From Roudier et al. (2020). concern the dynamics of granulation (Sec. 3.1), and its underly￾ing magnetism (Sec. 3.2), the measurement of electric currents (Sec. 3.3), the heating of the chromosphere (Sec. 3.4), the photo￾sphere induced coronal oscillations (Sec. 3.5), coronal rain (Sec. 3.6), the signature of flares and eruptions (Sec. 3.7), the solar wind h… view at source ↗
Figure 2
Figure 2. Figure 2: (Left panel) Disk-center emerging (bolometric) intensity from a radiation hydrodynamical simulation of solar granulation, performed with the Stagger-code on an 8 × 8 Mm domain (25 km grid resolution). (Right panel) Power spectrum of the intensity as a function of wavenumber (1/Mm). Colored straight lines indicate turbulence regimes, and vertical lines indicate characteristic physical scales at the solar su… view at source ↗
Figure 3
Figure 3. Figure 3: Distribution of the vertical component of the electric current density jz (left column), as well as their intensity difference (right col￾umn) before (top row) and after (bottom row) a major solar eruptions. Adapted from Janvier et al. (2016). Measuring electric currents and understanding their distribu￾tion (e.g. Bommier et al. 2007), has been a core theme of French solar physics research this past two de… view at source ↗
Figure 4
Figure 4. Figure 4: Shock locations in a QS coronal hole numerical Bifrost model. The left panels shows regions of compression (red) and expansion (green) in the chromosphere and highlights shock dynamics (purple). Magnetic field lines indicate the different configuration. The dashed line outlines a chromospheric shock region, close to the β = 1 surface, while arrows mark compression sites associated with wave propagation (bl… view at source ↗
Figure 6
Figure 6. Figure 6: Fine-scale coronal rain observed near the footpoint of large coronal loops with a ground-based telescope. Top panel: RGB im￾age combining one spectral band of SDO/AIA, Hα observations from SST/CRISP, and Ca II K observations from the SST/CHROMIS. Bot￾tom panel: Hα slice using the path (1) demarcated by dotted lines in the top panel. Six rain strands are clearly visible with widths of about 0.2 arcseconds (… view at source ↗
Figure 5
Figure 5. Figure 5: Zoom-in view of active region 13470 observed on October 2023 conjointly by SolO (left column) and SST (right column). The first row shows the photosphere in the continuum emissions of neutral iron, the second row the inferred line-of-sight magnetic field, and the third row the chromosphere in the Hα line core (right panel) and hot corona at 174Å. Figure taken from Poirier et al. (2025). in the chromosphere… view at source ↗
Figure 7
Figure 7. Figure 7: Two simulations using the OHM and AMRVAC codes of eruptive twisted flux tubes (right panels), and a comparison of the synthetic magnetograms (middle panels) with an SDO/HMI magnetogram (left) showing the “scar” of the sunspot (in dark, on the positive-polarity spots in white), identified through model–observation coupling as being located at the footpoints of the eruptive flux tubes (Xing et al. 2024b). (P… view at source ↗
Figure 8
Figure 8. Figure 8: Flux rope formation via sparse flux-cancellation in a Bifrost simulation. Top row show a time sequence of 3D rendering illustrating how a initially un-twisted magnetic field (top-left panel) can self-consistently turn into a flux-rope via granulation forcing. The bottom row illustrate photospheric magnetic maps of the vertical component Bz during this time sequence and highlights flux cancellations during … view at source ↗
Figure 9
Figure 9. Figure 9: Slow solar wind ISAM 1-D simulations including protons and alpha particles, compared to remote-sensing and in-situ measurements (see Lomazzi et al. 2026, for the latest results). PSP and SolO in-situ measurements are given for both protons (blue dots) and alpha particles (red dots). The various panels show respectively, the number density, the parallel and perpendicular component of the temperature (with r… view at source ↗
Figure 10
Figure 10. Figure 10: Fractionation of heavy ions in an active region loop modelled with the ISAM code. The plots show the deviation of atmospheric abundances from the photospheric (surface) values, where abundances are here taken relative to Oxygen. Left panel: Evolution of the fractionation with altitude. Right panel: Fractionation as a function of FIP, extracted at two heights in the ISAM simulations at the top of the chrom… view at source ↗
Figure 11
Figure 11. Figure 11: Example of predicted magnetic connectivity from the Earth to the Sun by the connectivity tool for November 5 2025 based on a low￾resolution magnetogram (GONG-ADAPT). The position of the Earth projected in Carrington coordinates is shown with a yellow triangle. The dark line indicates the Earth field of view. The estimated connectivity on the solar surface is shown with yellow circles. The uncertainties co… view at source ↗
Figure 12
Figure 12. Figure 12: Snapshots of the photospheric magnetic field associated to an active nest from February to July 2022. We combine here multi-view measurements from SDO/HMI and SO/PHI. Solar flares associated are shown with crosses coloured by flare class. When available, the NOAA active region numbers are annotated. The arrows highlight flux emergence between each snapshot. From Finley et al. (2025). regions merging than … view at source ↗
Figure 13
Figure 13. Figure 13: Snapshots of the multi-wavelength observation of an erupting filament in order to identify the corresponding CME parameters. Panel (b) shows the SDO/HMI magnetogram to identify the PIL and deduce the magnetic field inclination. Panel (c) shows a chromospheric image of SDO/AIA 304 to identify the shape of the flux rope and deduce its handedness. Panel (e) shows an EUV image by SDO/AIA 211 to identify the c… view at source ↗
Figure 14
Figure 14. Figure 14: Upper left panel (Adapted from Valori et al. 2023) : First fully-observational vector magnetic field map, with the ambiguity resolved thanks to the SDM method. Upper right panel (Adapted from Valori et al. 2023): comparison of the agreement on ambiguity of the transverse field of the SDM-disambiguated vector map with a vector map in which ambiguity is solved with a model-dependant method (minimum energy m… view at source ↗
Figure 15
Figure 15. Figure 15: Example of a NLFFF magnetic extrapolation from a photospheric vector magnetogram. Left panel: Transverse magnetic field of active region NOAA 10808 measured by THEMIS on 2005 September 13 at 15:25 UT, with overlaid contour levels of the normal magnetic field (at Bz = [0, ±400, ±800, and ± 1200] G). Right panel: set of field lines reconstructed with the XTRAPOL as using the THEMIS vector magnetogram as bou… view at source ↗
Figure 16
Figure 16. Figure 16: Illustrative image of how high-resolution observations obtained by EST (here HiFI/GREGOR Hα observation by Christoph Kuckein) can be used as inputs for numerical models of solar eruptions (Masson et al. 2019, here adapted from). Advancing the understanding of solar eruptions, being a fundamentally multi-scale process, requires both data of the source regions at the lowest possible scale, and numerical mod… view at source ↗
read the original abstract

The project of the European Solar Telescope aims to provide a state-of-the art infrastructure to study the Sun and its interactions with Earth and the heliosphere. This 4.2m aperture telescope will be equipped with multi conjugate adaptive optics, light-polarisation analyser, imaging spectrograph and integral field unit spectrographs. It will provide unprecedented observations of the solar photosphere and chromosphere and of the dynamical events and features that pertains to the low solar atmosphere. The EST project is presently in a phase of crystallisation, aiming at the creation of an European Research Infrastructure Consortium. While the French community has continuously been associated with the development of the EST project, some specific scientific aspects are more particularly relevant for the French astrophysics and heliophysics communities. The present review highlights the scientific research axes of high interest from the French community that shall strongly benefit from EST. The later will not only advance numerous topics of solar physics, as well as solar adaptive optics developments, but will also provide unrivaled datasets of high interest in the framework of space weather. This review also aims to highlight the space weather use that can be done with future EST observations, that will be particularly relevant for French heliophysicists.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. The manuscript is a white paper advocating for the European Solar Telescope (EST), a 4.2 m aperture facility equipped with multi-conjugate adaptive optics, light-polarisation analyser, imaging spectrograph and integral-field-unit spectrographs. It states that the project is currently in a crystallisation phase aimed at ERIC creation and argues that EST will deliver unprecedented observations of the solar photosphere and chromosphere together with unrivaled datasets of high interest for space weather. The paper highlights specific scientific research axes of particular relevance to the French heliophysics and astrophysics communities and notes ongoing French involvement in the project.

Significance. If the EST reaches full operation and French researchers obtain data access, the facility would supply high-resolution, multi-diagnostic observations that could advance studies of solar atmospheric dynamics, adaptive-optics techniques and space-weather forecasting, aligning with stated French community priorities. The document's primary value lies in community coordination and science-case articulation rather than new empirical results or derivations.

major comments (1)
  1. Abstract: all forward-looking claims that EST 'will provide unprecedented observations ... and unrivaled datasets' rest on the premise that the project will advance from its described crystallisation phase to construction, commissioning and data access for the French community; the manuscript supplies no risk assessment, timeline or contingency discussion for these steps, leaving the central advocacy conditional on an external premise that is not examined within the document.
minor comments (2)
  1. Abstract: 'The later will not only advance' should read 'The latter will not only advance' for grammatical clarity.
  2. Abstract: 'dynamical events and features that pertains to the low solar atmosphere' should read 'pertain' for subject-verb agreement.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their review and for recognizing the value of the white paper in articulating science cases and community priorities. We address the single major comment below.

read point-by-point responses

  1. Referee: [—] Abstract: all forward-looking claims that EST 'will provide unprecedented observations ... and unrivaled datasets' rest on the premise that the project will advance from its described crystallisation phase to construction, commissioning and data access for the French community; the manuscript supplies no risk assessment, timeline or contingency discussion for these steps, leaving the central advocacy conditional on an external premise that is not examined within the document.

    Authors: We acknowledge that the manuscript's forward-looking statements are conditional on the EST advancing beyond its current crystallisation phase. However, this document is a community white paper whose purpose is to outline the scientific relevance of EST for French heliophysics and space-weather research, not to serve as a project-management or risk-analysis report. The crystallisation phase and ERIC goal are stated explicitly, and the text focuses on the observational capabilities and French-relevant science axes that would become accessible if the facility is realized. Detailed timelines, contingencies, and risk assessments belong in dedicated EST project documentation rather than in a science-case white paper, which is the standard approach taken by similar community documents. We therefore see no need to expand the manuscript in this direction. revision: no

Circularity Check

0 steps flagged

No circularity; white paper is a review without derivations or reducible predictions

full rationale

The document is a white paper advocating for the European Solar Telescope, containing no equations, mathematical derivations, parameter fits, or predictions that reduce by construction to the paper's own inputs. Claims about future observations are forward-looking statements conditional on project progress, not derived results. No self-citation load-bearing steps, uniqueness theorems, or ansatzes appear. The paper is self-contained as a statement of community interest and is scored 0 per the default expectation for non-derivational manuscripts.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a white paper on infrastructure relevance with no mathematical claims, fitted parameters, or scientific derivations.

pith-pipeline@v0.9.1-grok · 6106 in / 877 out tokens · 25990 ms · 2026-06-25T23:07:59.735922+00:00 · methodology

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