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Detection of "diffuse" coronal He I 1083 during the April 8 2024 Solar Eclipse: evidence for terrestrial atmospheric scattering origin

T0 review · 3 major / 6 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read April 2024 eclipse data show the coronal helium line comes from Earth's atmosphere, not the Sun.

desk verdict Solid observational case against coronal He I 1083, but the title's scattering mechanism is a hypothesis without a quantitative estimate. read the letter →

arxiv 2501.01009 v2 pith:HMSNCW53 submitted 2025-01-02 astro-ph.SR

M. E. Molnar , R. Casini , P. Bryans , B. Berkey , K. Tyson This is my paper · ORCID
classification astro-ph.SR
keywords HeI1083nmtotalsolareclipsecoronalheliumterrestrialatmosphericscatteringspectroscopynear-infraredspectrographneutralcoronaPaschen-gamma
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

A dedicated near-infrared spectrograph observed the April 8, 2024 total solar eclipse and detected the helium line at 1083 nm both above the lunar limb and on the lunar disc. The paper argues that the line's presence on the lunar disc, its chromospheric thermal width, and its brightening toward the flash spectrum show it is sunlight scattered by Earth's atmosphere, not neutral helium in the corona. If correct, earlier eclipse detections of this line do not support the idea of abundant neutral helium in coronal plasma.

What carries the argument

The central object is the CHEESE slit spectrograph, whose 1 cm slit spans 58 arcminutes so it images the lunar disc and the corona simultaneously. The load-bearing physical mechanism is the double-scattering of the solar flash spectrum by Earth's atmosphere, previously demonstrated for blue chromospheric lines; the paper's evidence consists of the co-spatial appearance of He I 1083 and H I Paschen-γ on the lunar disc, their chromospheric line widths, and the intensity gradient toward the flash spectrum location at third contact.

What would settle it

Observe the same spectral region from a platform above most of Earth's atmosphere, such as a high-altitude balloon, during a future totality: if the 1083 nm signal on the lunar disc and in the corona disappears, the terrestrial scattering origin is confirmed; if it persists with coronal brightness, the solar-origin hypothesis is revived. A simpler test is to compute the expected Rayleigh-scattered intensity at 1083 nm under the eclipse geometry and compare it to the measured signal.

Watch

Extended reading notes

Core claim

The paper reports that CHEESE, a new grating spectrograph built for this purpose, detected the He I 1083 nm line, the Fe XIII 1074.7 nm coronal line, and the H I Paschen-γ 1093.8 nm chromospheric line during totality on April 8, 2024. The Fe XIII line appears only above the lunar limb, as a true coronal signal should, while the He I and H I lines appear both above the limb and on the lunar disc, with a thermal width corresponding to roughly $10^{5}$ K rather than coronal temperatures, and with intensity increasing toward the part of the sky nearest the flash spectrum. The authors conclude that the He I signal is not solar coronal emission but terrestrial atmospheric scattering of chromospheric flash-spectrum radiation, and that this removes the main eclipse-based evidence for abundant neutral helium in the corona.

Load-bearing premise

The whole terrestrial-scattering explanation rests on the assumption that the double-scattering process demonstrated for blue chromospheric lines also operates at 1083 nm with enough efficiency to produce the observed signal, an efficiency the paper does not compute.

Editorial extensions

If this is right

  • If the scattering origin is right, previous eclipse detections of 'diffuse' coronal He I 1083 no longer count as evidence of neutral helium in the corona.
  • He I 1083 cannot be used as a routine Hanle-effect coronal magnetometry diagnostic until the atmospheric contamination is removed or avoided.
  • Eclipse observations of near-infrared chromospheric lines must include a sky-scattering correction and be interpreted with flash-spectrum geometry in mind.
  • The Fe XIII 1074.7 nm line, detected only above the limb, remains a clean coronal signal in the same data set.
  • A balloon- or space-based eclipse observation can settle the question by measuring the line above the scattering atmosphere.

Reading between the lines

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

  • The same scattering contamination should affect other strong near-infrared chromospheric lines, such as the Paschen series, so eclipse spectra using those lines may need a similar subtraction.
  • Because elastic scattering preserves line width, the chromospheric thermal width of the detected He I line cannot by itself distinguish a solar from an atmospheric origin; the decisive evidence is spatial and temporal, not spectral.
  • The measured intensity gradient along the slit could be used to constrain the scattering phase function of the terrestrial atmosphere at 1083 nm, giving a quantitative test of the proposed mechanism.
  • If confirmed, the result would imply that reported coronal neutral-helium abundances from eclipse data are upper limits set by atmospheric scattering, shifting models of helium ionization in the corona.
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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

3 major / 6 minor

Summary. The manuscript describes near-infrared slit-spectrograph observations of the solar corona and lunar disc made with the new CHEESE instrument during the April 8, 2024 total solar eclipse from Dardanelle, Arkansas. During totality the authors detect Fe XIII 1074.7 nm only above the lunar limb, while He I 1083 nm and H I 1093.8 nm Paschen-gamma appear both in the corona and on the lunar disc. Gaussian fits give chromospheric-scale line widths for He I 1083 and coronal-scale widths for Fe XIII 1074.7 nm. Instrumental checks (a detector region not imaging the slit, laboratory bleed tests, on-disc scattered-light estimates) are used to argue against camera bleed and internal scattering. The authors conclude that the He I 1083 signal is not of coronal origin and hypothesize, following Stellmacher and Koutchmy (1974), that it arises from terrestrial atmospheric double scattering of the chromospheric flash spectrum.

Significance. If the result holds, it directly challenges the interpretation of earlier eclipse detections of 'diffuse' coronal He I 1083 as evidence for abundant neutral helium in the corona, and it sharpens the ongoing debate about the origin of this line in eclipse observations. The paper's main observational strengths are the simultaneous detection of a genuinely coronal line (Fe XIII 1074.7 nm) that is absent on the lunar disc, the on-disc calibration validating the spectral resolution, the spatial control provided by the non-slit region of the detector, and the public release of instrument designs and data. The central negative claim—that the observed He I 1083 is not evidence for coronal neutral helium—is well supported by the differential behavior of the three lines. The specific positive attribution to terrestrial atmospheric scattering is, however, asserted rather than quantitatively demonstrated, and this is the main weakness relative to the title claim.

major comments (3)
  1. [Abstract and Section 3, final paragraph] The title and abstract assert that the observations support a terrestrial atmospheric scattering origin for He I 1083, but no quantitative test of this mechanism is provided at 1083 nm. The comparison to Stellmacher and Koutchmy (1974) concerns blue chromospheric lines; Rayleigh scattering scales as lambda^-4, so the cross section at 1083 nm is roughly two orders of magnitude smaller than at 400 nm. Section 2.2 reports thin high cloud cover during totality, and the manuscript introduces no aerosol or cloud scattering component. To make the scattering attribution load-bearing, the authors should compute the expected scattered He I 1083 intensity (and its spatial gradient along the slit) from the flash-spectrum geometry and compare it with the observed counts, or explicitly quantify why the double-scattering mechanism remains efficient in the near-IR.
  2. [Section 3, dynamic-range discussion and Figure 4(f)] The camera's onboard processing reduced the effective dynamic range to 12 bits while the slit crossed bright chromospheric material, and the paper states that weak coronal signals fell outside the effective dynamic range. The line widths in Figure 4(f) are fitted from data taken in this regime. Because the measured chromospheric width of He I 1083 is a central discriminator, the manuscript needs to show that the dynamic-range compression does not significantly distort the fitted Gaussian widths and amplitudes, for example by injecting synthetic line profiles through the same onboard processing or by comparing widths measured before and after third contact when the illumination changed.
  3. [Section 3 and Figure 4(e)-(f)] The claim that the He I 1083 intensity increases toward the closest location of the flash spectrum is presented qualitatively. Given that this spatial gradient is one of the three pieces of evidence for the atmospheric-scattering hypothesis, it should be quantified: the authors should fit the intensity variation along the slit against the angular distance to the flash-spectrum source, and compare that gradient with the prediction of the proposed scattering model. As written, the gradient is consistent with the hypothesis but does not distinguish it from other non-coronal mechanisms.
minor comments (6)
  1. [Section 2.2] The phrase 'an anomalous vertical column shift (along the slit) on the left side of the detector' is unclear; it should specify whether the shift is in the dispersion direction or the slit direction, and how it was determined.
  2. [Figure 4 caption] The caption contains an incomplete sentence, 'In total we had.' This appears to be a leftover from an earlier draft and should be removed or completed.
  3. [Section 4] The sentence 'There are a few other plausible explanations for our observation, which need to be addressed in detail before rejected' should read 'before being rejected' or 'before they are rejected.'
  4. [Section 4] The reference to 'the previously observed lines of CaIIion in the blue part of the spectrum Migeotte & Rosen (1955)' is missing a comma and would benefit from a parenthetical citation format consistent with the rest of the text.
  5. [Section 3] The text says the same reduction steps were applied 'as for the data shown in Figure 1,' but the on-disc calibration data are shown in Figure 3; the cross-reference should be corrected.
  6. [Section 2.1] The predicted spectral resolution is quoted as R~9,600, while the on-disc calibration yields R~7,000; the paper should briefly explain the difference (for example, slit width, seeing, or focus) so that readers do not interpret it as an inconsistency.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the eclipse detection and the non-coronal interpretation rest on direct observations and an externally published line-width relation, not on fitted inputs or load-bearing self-citations.

full rationale

The paper's central claim is an observational one: He I 1083 and H I Paschen-gamma are detected on the lunar disc as well as in the corona, while Fe XIII 1074.7 nm appears only above the limb. This contrast is measured directly from the co-added eclipse frames and is not produced by any fitted parameter or by a prior result of the authors. The line-width interpretation uses Equation 14 from Schad et al. 2024, an external published relation, to convert measured Gaussian widths into temperatures; this is an interpretation of the data, not an input that predetermines the conclusion. The attribution to terrestrial atmospheric scattering is explicitly presented as a hypothesis supported by the presence of chromospheric lines on the lunar disc, the chromospheric line width, the intensity increase toward the flash-spectrum location, and the timing near third contact. The authors invoke Stellmacher & Koutchmy 1974, an independent external experiment, as the proposed mechanism; they do not fit a scattering model to the CHEESE data and then claim that fit as a prediction. The absence of a quantitative 1083 nm scattering intensity calculation is a limitation on the strength of the positive attribution, but it is not a circularity. The only self-citations (Molnar & Casini 2024, Casini et al. 2023, Khan et al. 2024) appear in the introduction as context for He I 1083 magnetometry and UV polarimetry and are not load-bearing for the eclipse detection or the scattering conclusion. No equation in the paper reduces to its own input, and no fitted parameter is renamed as a prediction. The derivation chain is therefore self-contained with respect to the paper's central observational finding; the interpretation is weaker than the detection, but that is an evidentiary concern, not circular reasoning.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

The central claim rests on no new physical entities and no ad hoc numbers. The free parameters are the standard Gaussian fits to the line profiles and the instrument line-spread width from the atlas fit; neither is adjusted to force the conclusion. The axioms are: thermal-broadening interpretation of line widths, lunar occultation geometry, the unquantified applicability of the 1974 scattering mechanism at 1083 nm, and the validity of the on-disc dispersion solution during the eclipse. The most fragile item is the scattering mechanism at near-IR wavelengths.

free parameters (2)
  • Gaussian line profile parameters (center, width, amplitude, linear background) for Fe XIII 1074.7, He I 1083, H I 1093.8 = Not tabulated; widths shown in Fig. 4(f)
    The inferred chromospheric temperature of the He I 1083 line (about 10^5 K) and the coronal temperature of Fe XIII (about 10^6 K) come from these fitted widths via Schad et al. (2024) Eq. 14.
  • Instrument line spread function width = R about 7000 from atlas fit (Fig. 3e)
    Free parameter in the solar-atlas fit used to verify the spectrograph resolution. Not load-bearing for the main conclusion since the He I versus Fe XIII width difference is large, but it is a fitted value used in instrument characterization.
assumptions (4)
  • domain assumption The observed line width is dominated by thermal Doppler broadening, and Eq. 14 of Schad et al. (2024) converts measured width to plasma temperature.
    Invoked in Section 3 to infer 10^5 K for He I 1083 and 10^6 K for Fe XIII. The paper's phrasing 'assuming no thermal Doppler broadening' is internally confusing and likely intended to mean no non-thermal broadening; either way, the thermal interpretation of the width is a domain assumption.
  • domain assumption The Moon occults all solar coronal emission at the lunar disc position, so He I 1083 detected in front of the lunar disc originates in the foreground (Earth's atmosphere or instrument).
    Standard astronomical fact used implicitly in Section 3 to argue that the He I 1083 signal on the lunar disc is not of solar origin.
  • domain assumption The Stellmacher and Koutchmy (1974) double-scattering mechanism for chromospheric flash-spectrum light applies to the near-IR lines at 1083 nm and 1093.8 nm with sufficient efficiency.
    Adopted in Sections 3 and 4 without a quantitative scattering calculation. This is the most fragile premise because the mechanism was validated for blue lines where Rayleigh scattering is far stronger.
  • domain assumption The wavelength dispersion solution from the on-disc calibration (13:23 UT) remains valid for the eclipse data (18:54 UT) despite repointing between calibrations.
    Section 3 states the eclipse data were reduced with the on-disc dispersion relation; the paper relies on the detected spectral lines matching the predicted wavelength positions (panels b-d of Fig. 4). Any flexure or thermal shift would move lines off the predicted locations.

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Cite this review

Pith. "Pith review of Detection of "diffuse" coronal He I 1083 during the April 8 2024 Solar Eclipse: evidence for terrestrial atmospheric scattering origin." pith.science (2026). https://pith.science/paper/HMSNCW53

@misc{pith2026250101009,
  author       = {Pith},
  title        = {Pith review of: Detection of "diffuse" coronal He I 1083 during the April 8 2024 Solar Eclipse: evidence for terrestrial atmospheric scattering origin},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HMSNCW53}},
  note         = {Machine review of arXiv:2501.01009}
}
read the original abstract

Strong He I 1083 nm atomic line signals have been previously measured during total solar eclipses at coronal heights above the lunar limb. This rather unexpected measurement has kindled a discussion about the hypothesized presence of significant amounts of neutral helium at coronal conditions. We performed spectroscopic observations of the He I 1083 nm spectroscopic region with the newly built CHEESE instrument during the April 8th 2024 total solar eclipse to test the presence of He I 1083 in the solar corona. We detected the He I 1083, the forbidden coronal line Fe XIII 1074.7 nm, as well as the chromospheric H I 1093.8 nm Paschen-{\gamma} line in our eclipse observations. The chromospheric He I 1083 and H I 1093.8 nm Paschen-{\gamma} lines are detected in the corona as well as on the lunar disc. Our findings point toward a non-solar origin of the He I 1083 signal during the April 8th 2024 eclipse that challenge the notion of abundant neutral helium in the solar corona inferred from eclipse observations.

Figures

Figures reproduced from arXiv: 2501.01009 by the authors.

Figure 1
Figure 1. Overview of the CHEESE instrument. Panel (a): Optical layout of the CHEESE instrument produced with the Zeemax software suite. The primary and secondary mirrors of the Skywatcher Quattro telescope correspond to M1 and M2, the diagonal 90◦ mirror to M3, and the two collimating lenses in the spectrograph are labeled as L1 and L2. Panel (b): CHEESE during laboratory bench assembly in NSF NCAR/HAO. The essential optical… view at source ↗
Figure 2
Figure 2. Composite context coronal images showing the position of the CHEESE slit during the eclipse campaign: Panel (a): solar disc data taken from SDO/AIA 1600 ˚A channel; the corona above 1.01 R⊙ is imaged by the MLSO/K-Cor white light coronograph on April 9 2024, the day after the eclipse. Panel (b): Solar disc taken from SDO/AIA 304 ˚A channel; the corona above is imaged in white light from Durango, Mexico; the image is… view at source ↗
Figure 3
Figure 3. Calibration on-disc data taken at 13:23 UT Apr 8 2024. Panel (a): Raw CHEESE spectrum in sensor coordinates. The X-direction corresponds roughly to the dispersion direc￾tion and the Y-axis to the slit direction. Panel (b): Slices through the spectrum of the disc (orange) and the sky (blue) (corresponding to the dashed lines in Panel (a)). Panel (c): Flat fielded, continuum normalized, and de-rotated CHEESE spectrum … view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: Results from the eclipse observations. Panel (a): Processed CHEESE spectrum obtained during the total solar eclipse between 11:54:17 - 11:54:28 UT on April 8th 2024. In total we had. Note the ever present He I 1083.0 nm line, as well as the Fe XIII 1074 nm line. A very…

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Forward citations

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Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.