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arxiv: 2605.21772 · v1 · pith:2T224MYCnew · submitted 2026-05-20 · 🌌 astro-ph.SR

Evidence for neutron capture in heavy-metal hot subdwarfs: Far-UV spectroscopy of EC22536-5304 and LSIV-14 116

M. Dorsch , C. S. Jeffery , J. Deprince , D. J. Dougan , S. Beauraind , H. Dupuis , T. Battich , P. Quinet
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U. Heber L. J. A. Scott S. Geier
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Pith reviewed 2026-05-22 07:43 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords hot subdwarfsheavy metal enrichmenti-processnucleosynthesisUV spectroscopyabundance analysisneutron capturestellar evolution
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The pith

The Pb-rich subdwarf EC22536-5304 shows an abundance pattern matching i-process nucleosynthesis, indicating self-enrichment via neutron capture.

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

This paper analyses the first far-ultraviolet spectra of two heavy-metal hot subdwarfs to measure abundances of many elements heavier than iron. The star EC22536-5304 reaches extreme overabundances that decline smoothly from strontium to bismuth in a way that matches the yields expected from the i-process. A reader would care because the pattern cannot be produced by diffusion or accretion alone and instead points to internal neutron-capture nucleosynthesis. The second star, LSIV-14 116, shows a different peak enrichment at lighter heavy elements, consistent with a separate formation path.

Core claim

EC22536-5304 reaches 6.2 dex enrichment in lead and 5.4 dex in bismuth relative to solar values. Its full abundance pattern from strontium through bismuth closely reproduces the predictions of i-process nucleosynthesis. This match supplies direct evidence that the heavy metals were produced by neutron capture inside the star. LSIV-14 116 instead peaks near 4.3 dex for strontium to tin and declines toward lead and bismuth, consistent with a different nucleosynthetic history.

What carries the argument

i-process nucleosynthesis pattern, a sequence of neutron-capture yields at intermediate neutron densities that reproduces the observed heavy-element abundances in EC22536-5304.

If this is right

  • The abundance patterns retain a clear nucleosynthetic signature that atomic diffusion alone cannot reproduce.
  • Heavy metals in other intermediate helium-rich sdOB stars are also likely self-synthesised.
  • EC22536-5304 probably formed through Roche-lobe overflow in a binary system.
  • LSIV-14 116 probably formed through the merger of two low-mass white dwarfs.

Where Pith is reading between the lines

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

  • The same i-process self-enrichment may operate in other classes of evolved stars that experience mixing episodes.
  • The newly computed atomic data for As III, Se III, Hf IV, Tl IV and Pb ions can now be applied to UV spectra of additional hot stars.
  • Stellar evolution models for low-mass helium-burning stars may need to incorporate i-process channels when binary interaction is present.

Load-bearing premise

The measured abundances reflect the star's nucleosynthetic history rather than being reshaped by atmospheric diffusion or other non-nuclear processes.

What would settle it

If revised non-LTE models using different atomic data or including full diffusion produce abundances for EC22536-5304 that no longer align with i-process predictions, the claimed match would be ruled out.

Figures

Figures reproduced from arXiv: 2605.21772 by C. S. Jeffery, D. J. Dougan, H. Dupuis, J. Deprince, L. J. A. Scott, M. Dorsch, P. Quinet, S. Beauraind, S. Geier, T. Battich, U. Heber.

Figure 1
Figure 1. Figure 1: The strongest Ga, Ge, Se, Kr, Sr, Y, and Zr lines in the STIS [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Top: the strongest Asiii-iv lines in LS IV−14◦116, with available oscillator strengths (see Fig. A.2 for Asiv lines with￾out). Bottom: similar for Br iv; note also Hg iv 1158.191 Å. See [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Nb (Z = 41), Mo (42), Pd (46), Cd (48), In (49), Sn (50), Te (52), I (53), and Xe (54) lines in LS IV−14◦116, like [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Possible detection of Ag iv in LS IV−14◦116, like [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Top: HFS splitting of Sb v 1226 Å in HD 127493, EC 22536−5304, and LS IV−14◦116. Split component wave￾lengths are indicated. The HFS splits are clearly resolved in HD 127493 because it was observed at R = 114 000. Bottom: the strongest Sb iv lines in LS IV−14◦116, like [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: The strongest La iv lines in EC 22536−5304, like [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Ce (Z = 58), Pr (59), Nd (60), Er (68), Yb (70), Lu (71), Hf (72), W (74), and Os (76) lines in EC 22536−5304, like [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: HFS-split Ta v lines in EC 22536−5304, similar to [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 10
Figure 10. Figure 10: The strongest Hg iv-v, Tl iv, Pb iii-vi, and Bi iii-v lines, next to Sn iv, in the STIS spectrum of EC 22536−5304; like [PITH_FULL_IMAGE:figures/full_fig_p015_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Top: Surface abundances of EC 22536−5304 and LS IV−14◦116 by number, compared to the solar pattern of Asplund et al. (2009), supplemented with heavy-metal results from Grevesse et al. (2015), Lodders (2019), and Asplund et al. (2021). Middle: Abundances relative to solar. Bottom: Solar-relative abundances, scaled to the same Fe abundance. Also shown are two models from Battich et al. (2025) with initial m… view at source ↗
Figure 12
Figure 12. Figure 12: Convection test for LS IV−14◦116 (red) and EC 22536- −5304 (blue). Top: Adiabatic gradients (solid), computed fol￾lowing Groth et al. (1985), compared with the Tlusty model gra￾dients (dashed); shaded regions indicate layers unstable accord￾ing to the Schwarzschild criterion. Bottom: UV line formation depths in EC 22536−5304; the strongest lines arise from C iii-iv, while most others are due to heavy meta… view at source ↗
read the original abstract

Most hot subdwarfs (sdO/B) are low-mass core-helium-burning stars formed through binary interaction. A subgroup of intermediate He-rich sdOBs shows extreme heavy-metal (Z>30) enrichments exceeding $10^4$ times solar, especially in Zr or Pb. We analyse the first ultraviolet spectra of the "heavy metal" subdwarfs LSIV-14 116 (Zr-rich) and EC22536-5304 (Pb-rich) to determine their abundance patterns and test nucleosynthesis models. Both stars show exceptionally rich heavy-element spectra dominated by ions in stages III-VI, many absent from standard line lists. We compiled literature energy levels, wavelengths, and oscillator strengths and implemented them in the SYNSPEC code. In addition, we computed new oscillator strengths for As III, Se III, Hf IV, and Tl IV. New photoionisation cross-sections for Pb III-VI enabled the first non-LTE models of multiply ionised Pb. In LSIV-14 116 we detect 16 light and 24 heavy metals (Ga-Bi); Br, Nb, Mo, Pd, In, Sb, Te, and Xe are measured in an sdO/B star for the first time. In EC22536-5304 13 light and 26 heavy metals are detected, including first detections of La, Ce, Pr, Nd, Er, Yb, Lu, Hf, Ta, W, Os, Pt, Hg, Tl, and Bi. LSIV-14 116 peaks at ~4.3 dex for Sr-Sn relative to solar, declining to 3.1 dex at Pb and 2.3 dex at Bi, whereas EC22536-5304 reaches 6.2 dex for Pb and 5.4 dex for Bi. Both stars are Fe-poor. The abundance patterns cannot be explained by atomic diffusion alone and retain a clear nucleosynthetic signature. EC22536-5304 closely matches predictions of i-process nucleosynthesis, providing strong evidence for i-process self-enrichment in hot subdwarfs. EC22536-5304 likely formed via Roche-lobe overflow, whereas LSIV-14 116 likely originated from the merger of two low-mass white dwarfs, which may explain differences in its enrichment pattern. These results suggest that heavy metals in other He-sdO/Bs may also be self-synthesised.

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

3 major / 3 minor

Summary. The manuscript presents far-UV spectroscopic analysis of two heavy-metal hot subdwarfs, LSIV-14 116 and EC22536-5304. It compiles atomic data, computes new oscillator strengths for several ions and photoionisation cross-sections for Pb, and uses non-LTE SYNSPEC models to derive abundances of light and heavy elements. The paper reports numerous first detections of heavy elements in these stars and concludes that the abundance pattern in EC22536-5304 closely matches i-process nucleosynthesis predictions, providing evidence for self-enrichment via neutron capture. Different formation channels are suggested for the two objects.

Significance. If the results hold, this paper would make a notable contribution to the field by offering direct evidence for i-process operation in hot subdwarfs, which are typically not associated with such nucleosynthesis. The first detections of elements such as Br, Nb, Mo, Pd, In, Sb, Te, Xe, La, Ce, Pr, Nd, Er, Yb, Lu, Hf, Ta, W, Os, Pt, Hg, Tl, and Bi in sdO/B stars are valuable additions to stellar abundance studies. The work also demonstrates the importance of updated atomic data for analyzing complex UV spectra.

major comments (3)
  1. [Atomic data compilation and calculations] The newly computed oscillator strengths for As III, Se III, Hf IV, and Tl IV, as well as the Pb III-VI photoionisation cross-sections, are critical for the non-LTE modeling and abundance derivations of the heavy elements. The manuscript does not include any external validation, laboratory comparisons, or sensitivity analyses for these data. This is a load-bearing issue because uncertainties of 0.3 dex or more in log gf values could significantly affect the reported Pb abundance of 6.2 dex and Bi of 5.4 dex, thereby impacting the claimed close match to i-process predictions.
  2. [Results and discussion for EC22536-5304] The statement that EC22536-5304 'closely matches predictions of i-process nucleosynthesis' is central to the paper's main conclusion. However, no quantitative measure of the fit (e.g., reduced chi-squared or element-by-element residuals with uncertainties) is provided, making it hard to evaluate how robust the match is against the derived abundance errors.
  3. [Abundance determination methods] The paper lacks a detailed error budget for the derived abundances, including contributions from atomic data uncertainties, model atmosphere assumptions, and line blending in the UV spectra. This omission makes it difficult to assess the reliability of the nucleosynthetic interpretation over alternative explanations like diffusion.
minor comments (3)
  1. [Abstract] The abstract could specify the wavelength range of the far-UV spectra analyzed for clarity.
  2. [Spectral figures] The spectral figures would benefit from annotations indicating which lines are from newly computed data versus literature values.
  3. [References] Ensure all relevant prior works on hot subdwarf abundances and i-process calculations are cited, particularly any recent studies on similar objects.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thorough and constructive review of our manuscript. We address each major comment below and will incorporate revisions to strengthen the paper.

read point-by-point responses

  1. Referee: [Atomic data compilation and calculations] The newly computed oscillator strengths for As III, Se III, Hf IV, and Tl IV, as well as the Pb III-VI photoionisation cross-sections, are critical for the non-LTE modeling and abundance derivations of the heavy elements. The manuscript does not include any external validation, laboratory comparisons, or sensitivity analyses for these data. This is a load-bearing issue because uncertainties of 0.3 dex or more in log gf values could significantly affect the reported Pb abundance of 6.2 dex and Bi of 5.4 dex, thereby impacting the claimed close match to i-process predictions.

    Authors: We agree that the presentation of the new atomic data would benefit from additional discussion of validation and uncertainties. The oscillator strengths were computed using the Hartree-Fock method with relativistic corrections, and the Pb photoionisation cross-sections were obtained via the R-matrix approach; limited internal comparisons to existing theoretical values were performed during the work. To address the referee's concern, we will add a dedicated subsection describing the computational methods, any available literature comparisons, and a sensitivity analysis quantifying the impact of plausible variations in log gf values on the derived Pb and Bi abundances. revision: yes

  2. Referee: [Results and discussion for EC22536-5304] The statement that EC22536-5304 'closely matches predictions of i-process nucleosynthesis' is central to the paper's main conclusion. However, no quantitative measure of the fit (e.g., reduced chi-squared or element-by-element residuals with uncertainties) is provided, making it hard to evaluate how robust the match is against the derived abundance errors.

    Authors: We concur that a quantitative metric would improve the robustness of this central claim. We will add a quantitative assessment of the fit, including computation of a reduced chi-squared value between the observed abundances and i-process model predictions, together with element-by-element residuals plotted or tabulated with their estimated uncertainties. revision: yes

  3. Referee: [Abundance determination methods] The paper lacks a detailed error budget for the derived abundances, including contributions from atomic data uncertainties, model atmosphere assumptions, and line blending in the UV spectra. This omission makes it difficult to assess the reliability of the nucleosynthetic interpretation over alternative explanations like diffusion.

    Authors: We will expand the methods and discussion sections to provide a detailed error budget. This will explicitly include estimated contributions from uncertainties in the new atomic data, variations in adopted model atmosphere parameters (Teff, log g, and microturbulence), and the effects of line blending in the far-UV region. The revised text will also address how these uncertainties influence the distinction between nucleosynthetic signatures and diffusion scenarios. revision: yes

Circularity Check

0 steps flagged

No circularity: abundances derived from spectra and matched to external i-process predictions

full rationale

The paper computes new oscillator strengths for As III, Se III, Hf IV, Tl IV and Pb photoionisation cross-sections, inserts them into SYNSPEC to generate non-LTE models, extracts observed abundances for 26 heavy elements in EC22536-5304, and reports that the resulting pattern closely matches independent i-process nucleosynthesis yields from the literature. No equation or step reduces the reported match to a fitted parameter inside the paper, a self-citation chain, or a redefinition of the input data. The nucleosynthesis comparison is presented as an external test rather than an internal consistency condition, and the atomic-data computations are described as enabling the measurement rather than being tuned to produce the target pattern. The derivation chain therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the accuracy of newly computed atomic data and on the assumption that the observed abundance pattern is dominated by nucleosynthesis rather than diffusion.

axioms (2)
  • domain assumption Standard non-LTE assumptions in stellar-atmosphere modeling apply to these stars.
    Invoked for the SYNSPEC non-LTE models of multiply ionized Pb.
  • domain assumption Compiled literature energy levels and the new oscillator strengths accurately represent the true atomic transitions.
    Required to identify lines and derive abundances for ions absent from standard lists.

pith-pipeline@v0.9.0 · 6057 in / 1495 out tokens · 68819 ms · 2026-05-22T07:43:03.592775+00:00 · methodology

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Works this paper leans on

208 extracted references · 208 canonical work pages · 1 internal anchor

  1. [1]

    & Reader, J

    Acquista, N. & Reader, J. 1980, Journal of the Optical Society of America (1917- 1983), 70, 789

    work page 1980

  2. [2]

    & Colón, C

    Alonso-Medina, A. & Colón, C. 2012, MNRAS, 427, 1312

    work page 2012

  3. [3]

    2011, Atomic Data and Nuclear Data Tables, 97, 36

    Alonso-Medina, A., Colón, C., & Porcher, P. 2011, Atomic Data and Nuclear Data Tables, 97, 36

    work page 2011

  4. [4]

    2009, MNRAS, 395, 567

    Alonso-Medina, A., Colón, C., & Zanón, A. 2009, MNRAS, 395, 567

    work page 2009

  5. [5]

    & Lindgard, A

    Andersen, T. & Lindgard, A. 1977, Journal of Physics B Atomic Molecular Physics, 10, 2359

    work page 1977

  6. [6]

    & Tauheed, A

    Ankita, S. & Tauheed, A. 2020, J. Quant. Spectr. Rad. Transf., 254, 107193

    work page 2020

  7. [7]

    H., Tauheed, A., & Kernahan, J

    Ansbacher, W., Pinnington, E. H., Tauheed, A., & Kernahan, J. A. 1991, Journal of Physics B Atomic Molecular Physics, 24, 587

    work page 1991

  8. [8]

    C., Christlieb, N., et al

    Aoki, W., Beers, T. C., Christlieb, N., et al. 2007, ApJ, 655, 492

    work page 2007

  9. [9]

    1930, Nature, 126, 565

    Arvidsson, G. 1930, Nature, 126, 565

    work page 1930

  10. [10]

    Arya, N. K. & Tauheed, A. 2020, J. Quant. Spectr. Rad. Transf., 255, 107253

    work page 2020

  11. [11]

    Arya, N. K. & Tauheed, A. 2022, J. Quant. Spectr. Rad. Transf., 292, 108353

    work page 2022

  12. [12]

    Arya, N. K. & Tauheed, A. 2023, European Physical Journal D, 77, 150

    work page 2023

  13. [13]

    M., & Grevesse, N

    Asplund, M., Amarsi, A. M., & Grevesse, N. 2021, A&A, 653, A141

    work page 2021

  14. [14]

    J., & Scott, P

    Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481

    work page 2009

  15. [15]

    I., Raassen, A

    Azarov, V . I., Raassen, A. J. J., Joshi, Y . N., Uylings, P. H. M., & Ryabtsev, A. N. 1997, Phys. Scr, 56, 325

    work page 1997

  16. [16]

    I., Raassen, A

    Azarov, V . I., Raassen, A. J. J., Wyart, J. F., Joshi, Y . N., & Churilov, S. S. 2000, Phys. Scr, 61, 133

    work page 2000

  17. [17]

    L., Pinnington, E

    Bahr, J. L., Pinnington, E. H., Kernahan, J. A., & O’Neill, J. A. 1982, Canadian Journal of Physics, 60, 1108

    work page 1982

  18. [18]

    M., Córsico, A

    Battich, T., Miller Bertolami, M. M., Córsico, A. H., & Althaus, L. G. 2018, A&A, 614, A136

    work page 2018

  19. [19]

    M., Serenelli, A

    Battich, T., Miller Bertolami, M. M., Serenelli, A. M., Justham, S., & Weiss, A. 2023, A&A, 680, L13

    work page 2023

  20. [20]

    M., Weiss, A., et al

    Battich, T., Miller Bertolami, M. M., Weiss, A., et al. 2025, A&A, 699, A298

    work page 2025

  21. [21]

    A., Romano, P., & Pradhan, A

    Bautista, M. A., Romano, P., & Pradhan, A. K. 1998, ApJS, 118, 259

    work page 1998

  22. [22]

    Beck, D. R. & Datta, D. 1991, Phys. Rev. A, 44, 758

    work page 1991

  23. [23]

    P., Chayer, P., Wesemael, F., et al

    Blanchette, J. P., Chayer, P., Wesemael, F., et al. 2008, ApJ, 678, 1329

    work page 2008

  24. [24]

    1995, A&AS, 110, 441

    Bonifacio, P., Castelli, F., & Hack, M. 1995, A&AS, 110, 441

    work page 1995

  25. [25]

    A., & Lugaro, M

    Brauner, M., Pignatari, M., Masseron, T., García-Hernández, D. A., & Lugaro, M. 2024, A&A, 690, A262

    work page 2024

  26. [26]

    M., Burbidge, G

    Burbidge, E. M., Burbidge, G. R., Fowler, W. A., & Hoyle, F. 1957, Reviews of Modern Physics, 29, 547

    work page 1957

  27. [27]

    Burke, P. G. 2011, R-Matrix Theory of Atomic Collisions, V ol. 61

    work page 2011

  28. [28]

    Busso, M., Gallino, R., & Wasserburg, G. J. 1999, ARA&A, 37, 239

    work page 1999

  29. [29]

    M., Jeffery, C

    Byrne, C. M., Jeffery, C. S., Tout, C. A., & Hu, H. 2018, MNRAS, 475, 4728

    work page 2018

  30. [30]

    W., Lugaro, M., & Karakas, A

    Campbell, S. W., Lugaro, M., & Karakas, A. I. 2010, A&A, 522, L6 Carvajal Gallego, H., Deprince, J., Berengut, J. C., Palmeri, P., & Quinet, P. 2023, MNRAS, 518, 332 Carvajal Gallego, H., Palmeri, P., & Quinet, P. 2021, MNRAS, 501, 1440

    work page 2010

  31. [31]

    1997, A&A, 321, 254

    Castelli, F., Parthasarathy, M., & Hack, M. 1997, A&A, 321, 254

    work page 1997

  32. [32]

    2006, Baltic Astronomy, 15, 131

    Chayer, P., Fontaine, M., Fontaine, G., Wesemael, F., & Dupuis, J. 2006, Baltic Astronomy, 15, 131

    work page 2006

  33. [33]

    2023, MN- RAS, 518, 368

    Chayer, P., Mendoza, C., Meléndez, M., Deprince, J., & Dupuis, J. 2023, MN- RAS, 518, 368

    work page 2023

  34. [34]

    Chayer, P., Vennes, S., Dupuis, J., & Kruk, J. W. 2005, ApJ, 630, L169

    work page 2005

  35. [35]

    Chikh, A., Deghiche, D., Meftah, A., et al. 2021, J. Quant. Spectr. Rad. Transf., 272, 107796 Article number, page 22 of 30 M. Dorsch et al.: Evidence for neutron capture in heavy-metal hot subdwarfs

    work page 2021

  36. [36]

    Churilov, S. S. & Joshi, Y . N. 1996, Journal of the Optical Society of America B Optical Physics, 13, 11

    work page 1996

  37. [37]

    S., Kildiyarova, R

    Churilov, S. S., Kildiyarova, R. R., & Joshi, Y . N. 1996, Canadian Journal of Physics, 74, 145 Colón, C. & Alonso-Medina, A. 2010, Journal of Physics B Atomic Molecular Physics, 43, 165001 Colón, C., Alonso-Medina, A., & Porcher, P. 2014, Atomic Data and Nuclear Data Tables, 100, 272

    work page 1996

  38. [38]

    Cowan, R. D. 1973, Nuclear Instruments and Methods, 110, 173

    work page 1973

  39. [39]

    Cowan, R. D. 1981, The theory of atomic structure and spectra

    work page 1981

  40. [40]

    Crooker, A. M. & Joshi, Y . N. 1964, Journal of the Optical Society of America (1917-1983), 54, 553

    work page 1964

  41. [41]

    2019, MNRAS, 488, 2503

    Cunningham, T., Tremblay, P.-E., Freytag, B., Ludwig, H.-G., & Koester, D. 2019, MNRAS, 488, 2503

    work page 2019

  42. [42]

    Curtis, L. J. 1992, Journal of the Optical Society of America B Optical Physics, 9, 5

    work page 1992

  43. [43]

    2026, arXiv e-prints, arXiv:2601.02250

    Dawson, H., Dorsch, M., Geier, S., et al. 2026, arXiv e-prints, arXiv:2601.02250

    work page arXiv 2026

  44. [44]

    2024, A&A, 686, A25 de Andrés-García, I., Alonso-Medina, A., & Colón, C

    Dawson, H., Geier, S., Heber, U., et al. 2024, A&A, 686, A25 de Andrés-García, I., Alonso-Medina, A., & Colón, C. 2016, MNRAS, 455, 1145 de Andrés-García, I., Colón-Ruiz, C., & Colón, C. 2019, ApJ, 870, 131 De Smedt, K., Van Winckel, H., Kamath, D., et al. 2016, A&A, 587, A6

    work page 2024

  45. [45]

    2024, PhD thesis, Friedrich Alexander University of Erlangen-

    Dorsch, M. 2024, PhD thesis, Friedrich Alexander University of Erlangen-

    work page 2024

  46. [46]

    S., & Scott, L

    Dorsch, M., Heber, U., Jeffery, C. S., & Scott, L. 2022, From atomic physics to stellar evolution: decoding the heavy-metal subdwarfs with HST, HST Pro- posal. Cycle 30, ID. #17072

    work page 2022

  47. [47]

    S., Irrgang, A., Woolf, V ., & Heber, U

    Dorsch, M., Jeffery, C. S., Irrgang, A., Woolf, V ., & Heber, U. 2021, A&A, 653, A120

    work page 2021

  48. [48]

    2019, A&A, 630, A130

    Dorsch, M., Latour, M., & Heber, U. 2019, A&A, 630, A130

    work page 2019

  49. [49]

    2020, A&A, 643, A22

    Dorsch, M., Latour, M., Heber, U., et al. 2020, A&A, 643, A22

    work page 2020

  50. [50]

    J., Dorsch, M., Scott, L

    Dougan, D. J., Dorsch, M., Scott, L. J. A., et al. 2025, MNRAS, 544, 4353

    work page 2025

  51. [51]

    Dutta, N. N. & Majumder, S. 2011, ApJ, 737, 25

    work page 2011

  52. [52]

    N., Roy, S., Dixit, G., & Majumder, S

    Dutta, N. N., Roy, S., Dixit, G., & Majumder, S. 2013, Phys. Rev. A, 87, 012501

    work page 2013

  53. [53]

    G., Grant, I

    Dyall, K. G., Grant, I. P., Johnson, C. T., Parpia, F. A., & Plummer, E. P. 1989, Computer Physics Communications, 55, 425

    work page 1989

  54. [54]

    A., Safronova, U

    Dzuba, V . A., Safronova, U. I., & Johnson, W. R. 2003, Phys. Rev. A, 68, 032503

    work page 2003

  55. [55]

    2013, Journal of Physics B Atomic Molecular Physics, 46, 095001

    Ekman, J., Grumer, J., Hartman, H., & Jönsson, P. 2013, Journal of Physics B Atomic Molecular Physics, 46, 095001

    work page 2013

  56. [56]

    2021, MNRAS, 503, 5730

    Elabidi, H. 2021, MNRAS, 503, 5730

    work page 2021

  57. [57]

    S., Belhadj, W., & Hamdi, R

    Elabidi, H., Sahal-Bréchot, S., Dimitrijevi ´c, M. S., Belhadj, W., & Hamdi, R. 2023, MNRAS, 522, 819

    work page 2023

  58. [58]

    Elias, L. R. 1972, PhD thesis, University of Wisconsin, Madison Enzonga Yoca, S., Palmeri, P., Quinet, P., Jumet, G., & Biémont, É. 2012a, Jour- nal of Physics B Atomic Molecular Physics, 45, 035002 Enzonga Yoca, S. & Quinet, P. 2013, Journal of Physics B Atomic Molecular Physics, 46, 145003 Enzonga Yoca, S. & Quinet, P. 2014, Journal of Physics B Atomic ...

    work page 1972

  59. [59]

    Epstein, G. L. & Reader, J. 1976, Journal of the Optical Society of America (1917-1983), 66, 590

    work page 1976

  60. [60]

    Epstein, G. L. & Reader, J. 1979, Journal of the Optical Society of America (1917-1983), 69, 511

    work page 1979

  61. [61]

    1930, Zeitschrift fur Physik, 60, 320 Fernández-Menchero, L., Jeffery, C

    Fermi, E. 1930, Zeitschrift fur Physik, 60, 320 Fernández-Menchero, L., Jeffery, C. S., Ramsbottom, C. A., & Ballance, C. P. 2020, MNRAS, 496, 2558

    work page 1930

  62. [62]

    2006, Journal of Physics : B Atomic Molecular and Optical Physics, 39

    Fivet, V ., Quinet, P., Biémont, E., & Xu, H.-L. 2006, Journal of Physics : B Atomic Molecular and Optical Physics, 39

    work page 2006

  63. [63]

    & Chayer, P

    Fontaine, G. & Chayer, P. 1997, in The Third Conference on Faint Blue Stars, ed. A. G. D. Philip, J. Liebert, R. Saffer, & D. S. Hayes, 169

    work page 1997

  64. [64]

    & Saxena, K

    Fraga, S. & Saxena, K. 1976, Handbook of Atomic Data (Elsevier Amsterdam)

    work page 1976

  65. [65]

    1996, A&A, 313, 497

    Freytag, B., Ludwig, H.-G., & Steffen, M. 1996, A&A, 313, 497

    work page 1996

  66. [66]

    Gautam, M. S. & Joshi, Y . N. 1972, Canadian Journal of Physics, 50, 2059

    work page 1972

  67. [67]

    N., Raassen, A

    Gayasov, R., Joshi, Y . N., Raassen, A. J. J., & Kaufman, V . 2000, Phys. Scr, 61, 164

    work page 2000

  68. [68]

    Grevesse, N., Scott, P., Asplund, M., & Sauval, A. J. 2015, A&A, 573, A27

    work page 2015

  69. [69]

    G., Kudritzki, R

    Groth, H. G., Kudritzki, R. P., & Heber, U. 1985, A&A, 152, 107

    work page 1985

  70. [70]

    1969, PhD thesis, University of British Columbia

    Gutmann, F. 1969, PhD thesis, University of British Columbia

    work page 1969

  71. [71]

    S., & Sahal-Bréchot, S

    Hamdi, R., Ben Nessib, N., Dimitrijevi´c, M. S., & Sahal-Bréchot, S. 2013, MN- RAS, 431, 1039

    work page 2013

  72. [72]

    J., Lugaro, M., & Meyer, B

    Hampel, M., Stancliffe, R. J., Lugaro, M., & Meyer, B. S. 2016, ApJ, 831, 171

    work page 2016

  73. [73]

    Han, Z., Podsiadlowski, P., Maxted, P. F. L., Marsh, T. R., & Ivanova, N. 2002, MNRAS, 336, 449

    work page 2002

  74. [74]

    & Tauheed, A

    Haris, K. & Tauheed, A. 2012, Phys. Scr, 85, 055301

    work page 2012

  75. [75]

    2009, ARA&A, 47, 211

    Heber, U. 2009, ARA&A, 47, 211

    work page 2009

  76. [76]

    2016, PASP, 128, 082001

    Heber, U. 2016, PASP, 128, 082001

    work page 2016

  77. [77]

    Encyclopedia of Astrophysics (chapter) , keywords =

    Heber, U. 2024, arXiv e-prints, arXiv:2410.11663

    work page arXiv 2024

  78. [78]

    R., et al

    Herwig, F., Pignatari, M., Woodward, P. R., et al. 2011, ApJ, 727, 89

    work page 2011

  79. [79]

    R., Lin, P.-H., Knox, M., & Fryer, C

    Herwig, F., Woodward, P. R., Lin, P.-H., Knox, M., & Fryer, C. 2014, ApJ, 792, L3

    work page 2014

  80. [80]

    M., Beers, T

    Holmbeck, E. M., Beers, T. C., Roederer, I. U., et al. 2018, ApJ, 859, L24

    work page 2018

Showing first 80 references.