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arxiv: 2606.23456 · v1 · pith:RS2346MRnew · submitted 2026-06-22 · 🌌 astro-ph.SR · astro-ph.GA

Stellar winds of O-type stars traced by high ionization fine-structure emission lines with JWST/MIRI

Calum Hawcroft , David R. Law , Linda J. Smith , Alexander W. Fullerton , Karl D. Gordon , Paul A. Crowther , Marjorie Decleir , Sascha T. Zeegers
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Christiana Erba Richard Ignace D. John Hillier
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Pith reviewed 2026-06-26 07:07 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA
keywords stellar windsO-type starsJWSTMIRIfine-structure lines[Ne V]mass lossterminal velocity
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The pith

JWST/MIRI observations of [Ne V] lines measure wind speeds in O-type stars.

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

The paper uses JWST/MIRI to search for high ionization fine-structure emission lines in 22 OB-type stars. It finds broad flat-topped [Ne V] 14.3 micron emission in five O-type stars, allowing measurement of terminal wind speeds and lower limits on mass-loss rates. These speeds generally follow empirical trends but can be lower than expected in some cases. The work shows that such MIR emission is common even in weak-wind O stars, providing a new diagnostic at higher ionization and longer wavelengths than standard methods.

Core claim

Broad, flat-topped emission in the [Ne V] 14.3 micron fine-structure line is detected in five O-type stars, from which terminal wind speeds are derived that generally agree with empirical trends, though some are surprisingly low, and lower limits on mass-loss rates are estimated. This establishes MIR fine-structure lines as a new probe of stellar winds formed at high ionization and large spatial extent, with frequent incidence in the sample including weak-wind stars.

What carries the argument

The broad, flat-topped profile of the [Ne V] 14.3 micron fine-structure emission line that traces the terminal wind velocity.

If this is right

  • Terminal wind speeds can be measured in O-type stars using mid-infrared observations.
  • Lower limits on mass-loss rates are obtainable from these lines for stars where other diagnostics fail.
  • High ionization lines provide wind information at larger spatial extents than UV or optical lines.
  • The method reveals wind emission in the weak-wind regime where it is often undetected otherwise.

Where Pith is reading between the lines

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

  • Similar observations could map the radial structure of winds by comparing lines formed at different distances.
  • This may help reconcile differences in mass-loss rate estimates from various wavelength regimes.
  • Extending the sample with more JWST data could test if low wind speeds correlate with specific stellar parameters.

Load-bearing premise

The [Ne V] 14.3 micron emission is produced in the stellar wind and its flat-topped shape directly corresponds to the terminal velocity without contamination from other regions.

What would settle it

High-resolution spectra revealing peaked rather than flat-topped [Ne V] line profiles or emission originating outside the wind in the same stars.

Figures

Figures reproduced from arXiv: 2606.23456 by Alexander W. Fullerton, Calum Hawcroft, Christiana Erba, David R. Law, D. John Hillier, Karl D. Gordon, Linda J. Smith, Marjorie Decleir, Paul A. Crowther, Richard Ignace, Sascha T. Zeegers.

Figure 1
Figure 1. Figure 1 [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: HRD showing the full sample discussed in this work. Symbols in green have sufficient S/N to allow us to make some comment on the nature of the line detection, those in red have very poor S/N. Filled symbols indicate a detection in [Ne v] 14.3µm, those filled with a lighter color are the tentative detections and open symbols are non-detec￾tions. Shapes indicate the luminosity class, circles for dwarf stars … view at source ↗
Figure 4
Figure 4. Figure 4: Mass-loss rates as a function of luminosity for the 5 stars with strong [Ne v] detections, shown as green circles. Black markers show a sample of Galactic O-type stars from T. Repolust et al. (2004); F. Martins et al. (2005b); P. A. Crowther et al. (2006) for comparison. Circles, triangles and squares correspond to luminosity classes V, III and I respec￾tively. Solid and dashed lines show theoretical mass-… view at source ↗
Figure 5
Figure 5. Figure 5: Ionization fraction q as a function of mass-loss rate for Ne4+. All curves are with an electron temperature of Te = 35kK. Vertical ticks show theoretical mass-loss rate pre￾dictions from R. Bj¨orklund et al. (2021), dashed, J. Krtiˇcka & J. Kub´at (2017), dotted and J. S. Vink et al. (2000), solid. estimate the mass-loss rates required to drive the ob￾served line flux in [Ne v]14.3 µm. Using these rela￾tio… view at source ↗
Figure 6
Figure 6. Figure 6: Left panel: Density profiles G(θ) as a function of the polar angle θ. Right panel: Continuum-subtracted profiles of fine-structure lines that would be seen by a distant observer as a function of the viewing inclination i. Labels within each panel list the stars whose spectra are statistically consistent with the computed profile [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
read the original abstract

We investigate the presence of high ionization fine-structure emission lines across a range of 22 OB-type stars observed with JWST-MIRI as part of calibration programmes and the WISCI and MEAD projects. MIR wind emission is detected in 4 late O-dwarfs (O8 V - O9 V), 1 early O-dwarf (O5 V) and there are tentative detections in an additional 3 stars (O8.5 II, O8.5 IV and O9 I). We measure the wind speeds and make estimates of lower limits on the mass-loss rates of 5 O-type stars from broad, flat-topped emission in the fine-structure line of [Ne V] 14.3micron. We find terminal wind speeds that are generally in agreement with empirical trends, but note that in some cases the wind speeds are surprisingly low. We highlight two main takeaways from this sample, which combine to establish an exciting new window into the winds of massive stars. First, a new diagnostic ability is gained from lines formed at much higher ionization, larger spatial extent, and longer wavelengths than typical wind diagnostics. Secondly, there is frequent incidence of MIR emission in O-type stars, even in the 'weak-wind' regime where wind emission is often not detected in the UV and optical.

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

2 major / 2 minor

Summary. The manuscript reports JWST/MIRI observations of 22 OB-type stars, detecting high-ionization fine-structure lines including [Ne V] 14.3μm in 5 O-type stars (4 late O-dwarfs, 1 early O-dwarf) with tentative detections in 3 more. Terminal wind speeds are derived from the widths of broad, flat-topped profiles for these 5 stars, generally consistent with empirical trends but with some noted as surprisingly low; lower limits on mass-loss rates are also estimated. The work positions these MIR lines as a new diagnostic for stellar winds at higher ionization and larger spatial scales, emphasizing their frequent incidence even among weak-wind stars.

Significance. If the line-profile interpretation holds, the result would establish a valuable new observational window into massive-star winds using high-ionization fine-structure lines at longer wavelengths, complementing UV/optical diagnostics and potentially constraining mass loss in the weak-wind regime where traditional tracers are often absent. The use of lines formed over larger spatial extents is a clear strength.

major comments (2)
  1. [line-profile analysis and discussion sections] The central claim that the observed flat-topped [Ne V] 14.3μm profiles directly yield terminal velocities (2 × v_∞) without substantial non-wind contamination is load-bearing for both the velocity measurements and the 'surprisingly low' cases. No quantitative radiative-transfer modeling, multi-epoch verification, or spatial information is supplied to exclude contributions from nebular, circumstellar, or ISM gas (see the line-profile analysis and discussion sections).
  2. [sample description and conclusions] The claim of 'frequent incidence' of MIR wind emission even in the weak-wind regime rests on a sample drawn from calibration programmes and the WISCI/MEAD projects. Post-selection of stars showing emission is not quantitatively assessed for bias, which directly affects the incidence statement (see the sample description and conclusions).
minor comments (2)
  1. [methods] Data-reduction steps, line-fitting procedures, and error propagation for the velocity and mass-loss estimates should be expanded with explicit equations or pseudocode for reproducibility.
  2. [figures] Figure captions for the line profiles would benefit from explicit velocity-scale annotations and direct overlays of the adopted terminal-velocity markers.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. We address each major point below and indicate the revisions we will make to strengthen the manuscript.

read point-by-point responses

  1. Referee: [line-profile analysis and discussion sections] The central claim that the observed flat-topped [Ne V] 14.3μm profiles directly yield terminal velocities (2 × v_∞) without substantial non-wind contamination is load-bearing for both the velocity measurements and the 'surprisingly low' cases. No quantitative radiative-transfer modeling, multi-epoch verification, or spatial information is supplied to exclude contributions from nebular, circumstellar, or ISM gas (see the line-profile analysis and discussion sections).

    Authors: We acknowledge that the velocity derivation assumes the flat-topped profiles arise from optically thin wind emission with the full width corresponding to 2 v_∞, without new radiative-transfer calculations in this work. The high ionization stage of [Ne V] makes substantial nebular or ISM contamination improbable, as these environments lack the required ionization. The profile morphology matches expectations from prior wind studies. We will revise the line-profile analysis and discussion sections to add explicit caveats on the assumptions, discuss possible contamination channels with supporting references, and qualify the 'surprisingly low' velocities accordingly. revision: partial

  2. Referee: [sample description and conclusions] The claim of 'frequent incidence' of MIR wind emission even in the weak-wind regime rests on a sample drawn from calibration programmes and the WISCI/MEAD projects. Post-selection of stars showing emission is not quantitatively assessed for bias, which directly affects the incidence statement (see the sample description and conclusions).

    Authors: The 22 OB stars were observed as part of calibration programmes and the WISCI/MEAD projects; target selection was independent of wind properties or prior emission-line detections. The reported incidence therefore reflects the fraction showing [Ne V] emission within this specific observed sample rather than a post-selected subset. We will revise the sample description to state the selection criteria explicitly and update the conclusions to qualify the incidence statement as applying to the observed sample, while noting the limitations for broader population inferences. revision: yes

Circularity Check

0 steps flagged

No circularity: direct observational measurements from line profiles compared to external trends.

full rationale

The paper reports direct measurements of terminal wind speeds from the observed widths of flat-topped [Ne V] 14.3 μm emission profiles in JWST/MIRI spectra of O-type stars, with lower limits on mass-loss rates also derived from these detections. These quantities are extracted from the data without any fitting of parameters that are then re-used as predictions of the same quantities. Comparisons are made to independent empirical trends from prior literature (not self-citations). No equations, ansatzes, or uniqueness theorems are invoked that reduce the reported results to the input data by construction. The central claims remain self-contained observational results.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; no explicit free parameters, axioms, or invented entities are stated. Measurements implicitly rely on standard assumptions in stellar wind spectroscopy (e.g., Sobolev approximation for line formation, terminal velocity law) but these are not detailed.

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