pith. sign in

arxiv: 2605.20360 · v1 · pith:ZTMCJ2COnew · submitted 2026-05-19 · 🌌 astro-ph.SR · astro-ph.GA· astro-ph.HE

The Highly Variable Wind from WD J005311, the Stellar Remnant of the Peculiar Galactic Supernova of 1181

C. Alexander Thomas , Peter Garnavich , Charlotte Wood , Richard Pogge , Lara Arielle Phillips This is my paper

Pith reviewed 2026-05-21 07:03 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GAastro-ph.HE
keywords white dwarfsupernova remnantline profile variationsO VI emissionrigidly rotating magnetospherestellar windWD J005311photometric variability
0
0 comments X

The pith

Spectroscopy of the 1181 supernova remnant shows O VI line profile variations arising from both a line-driven wind and an unstable rigidly rotating magnetosphere disk.

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

The paper reports time-resolved spectroscopy of WD J005311, the merged white dwarf left by the peculiar Galactic supernova observed in 1181. It identifies two distinct types of variability in the strong O VI emission line: broad line profile variations with amplitudes of about ten percent of the total flux that span the entire line, and narrower, lower-amplitude variations confined to the central plus or minus five thousand kilometers per second. The broad changes are attributed to instabilities in a line-driven wind, while the narrow features are linked to an unstable disk that forms in the rigidly rotating magnetosphere of the white dwarf. Archival near-ultraviolet photometry reveals a pseudo-periodic signal on roughly hourly timescales that may trace the breakout instability of this disk.

Core claim

Time-resolved spectroscopy reveals that the O VI emission line in WD J005311 shows broad line profile variations with amplitudes of ±10% of the line flux over the entire line, likely due to instabilities in the line-driven wind, and low-amplitude narrow LPVs within ±5000 km/s associated with an unstable disk formed from the rigidly rotating magnetosphere of the remnant white dwarf. Archival near-ultraviolet photometry indicates a pseudo-periodic oscillation with an hour-long timescale possibly from the breakout instability of this RRM disk.

What carries the argument

Line profile variations (LPVs) on two velocity scales in the O VI emission line, with broad changes tied to wind instabilities and narrow changes tied to an unstable disk in the rigidly rotating magnetosphere.

If this is right

  • Broad LPVs across the full O VI line arise from instabilities in the line-driven wind similar to those in Wolf-Rayet stars.
  • Narrow LPVs within the central velocity range trace an unstable disk formed by the rigidly rotating magnetosphere.
  • The hour-scale photometric oscillation may result from the breakout instability of the RRM disk.
  • Coherent structure in the broad LPVs is consistent with rotation on a roughly two-hour timescale, though individual features do not persist for a full cycle.

Where Pith is reading between the lines

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

  • Confirmation of the RRM disk would imply that the white dwarf retains a strong magnetic field and rapid rotation inherited from the white-dwarf merger event.
  • Similar dual-scale variability might appear in other post-merger white dwarfs that also drive line-driven winds.
  • The hourly photometric signal offers an independent way to constrain the disk's dynamical timescale without relying solely on spectroscopy.

Load-bearing premise

The narrow line profile variations are produced by an unstable disk that forms in the rigidly rotating magnetosphere of the merged white dwarf.

What would settle it

A direct measurement of the white dwarf's magnetic field strength or rotation period that is inconsistent with the velocity scale of the narrow LPVs at ±5000 km/s.

Figures

Figures reproduced from arXiv: 2605.20360 by C. Alexander Thomas, Charlotte Wood, Lara Arielle Phillips, Peter Garnavich, Richard Pogge.

Figure 1
Figure 1. Figure 1: Spectra of J0053 from 3200 ˚A to near-infrared wavelengths. The IR spectra were taken in the J, H, and K atmospheric windows and displayed as red lines. Weak emission features are detected in the near-IR, but are cutoff in these narrow bands due to their high Doppler widths. The average LBT/MODS spectrum from 10/16/2022 is shown as a blue line. The dotted line shows a hot black body with dust extinction of… view at source ↗
Figure 3
Figure 3. Figure 3: The average line profile of O VI feature for each night. For clarity, the spectra have been offset vertically. Narrow interstellar calcium “H+K” absorption lines are seen on the red side of the broad emission. Variations in line shape at the ±10% level are seen on time-scales of days to months, but no periodic pattern is seen. The LBT near-IR spectra are shown in [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 2
Figure 2. Figure 2: The O VI emission line profile from the average of the individual Keck spectra. The velocity is relative to the assumed rest wavelength of 3822 ˚A. The blue line shows the blue-shifted side of the line and the red is the shows the red-shifted side (note the two narrow interstellar Ca II absorption lines). The gray band shows the line profile from a simple wind model where the flux falls off as (v∞/v) 2 . v… view at source ↗
Figure 4
Figure 4. Figure 4: Top: The NUV O V emission line from the HST observations. The first visit is shown in blue and the second, two days later, is displayed in red. Narrow interstellar ab￾sorption lines of Mg II and Mg I are present. Reddening from dust combined with additional emission from Ne VIII results in the emission appearing to rise toward the red. The lower panel shows the percent difference in the line flux between t… view at source ↗
Figure 5
Figure 5. Figure 5: , where three representative O VI line profiles covering 1.5 hours are compared [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: The residual time series spectra of J0053 for each long time-series from the LBT. Along the x-axis is the velocity in 1000 km/s from the central wavelength of the O VI feature (3822 ˚A), the y-axis shows time since the first observation in minutes, and the color bar represents the relative intensity of the deviations from the average spectra for that night. length of the observations. Accelerating features… view at source ↗
Figure 7
Figure 7. Figure 7: Instantaneous spectral variation gradient time series of J0053 for each night of the LBT data. In contrast to [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: From left to right: the residual time series for the Keck observations, the instantaneous spectral variation gradient time series for the Keck observations, the scalogram of the wavelet transform of the Keck observations. broad fluctuations appear to weaken toward the center of the O VI line. 7 . One striking feature of the scalograms is the isolation of the narrow features in σ and line velocity. The resi… view at source ↗
Figure 9
Figure 9. Figure 9: Scalogram plots of the wavelet transform of the residual time series for each LBT dataset. The x-axis displays the velocity relative to the O VI rest wavelength of 3822˚A, and the y-axis shows the wavelet scale in km s−1 . The color represents the relative amplitude of the wavelet signal. 4. DISCUSSION 4.1. Broad LPVs from the Wind 4.1.1. Possible Coherent Features in the Time-Series A rotating star with l… view at source ↗
Figure 11
Figure 11. Figure 11: A comparison between the Keck gradient time-series and a gradient created from a simulated rotat￾ing shell. The shell has a random distribution of bright and dark spots that make one full rotation over the time-series. congruent with the data and suggests an periodicity of about 2 hours. We note that the rotational period of the stellar rem￾nant is predicted to be tens of seconds to a few minutes (Zhong e… view at source ↗
Figure 10
Figure 10. Figure 10: Top: Periodogram of the full STIS NUV light curve constructed with 1 s bins. The dotted red line indicates the power required for a 3σ detection of a periodic signal. The inset displays the frequency region zoomed-in on the power peak at 16.7 cycles d−1 . Over-plotted in red is the window function resulting from the combination of the two HST visits separated by 48 hr. Bottom: The STIS NUV light curve ave… view at source ↗
Figure 12
Figure 12. Figure 12: Four epochs from the LBT spectral series ob￾tained 01/04/2021. Each panel is an average of three con￾secutive residual spectra and the time shown is UT of the middle spectrum. Solid blue lines are the data and the light red line shows simulated pairs of O VI doublet emis￾sion features. Simulated doublets are Gaussian profiles with widths of 700 km s−1 (FWHM) and separated by a fixed 1800 km s−1 . The narr… view at source ↗
Figure 13
Figure 13. Figure 13: Top: The wavelet scalogram of 60 instanta￾neous gradient spectra observed under good seeing condi￾tions. The broad LPVs have been suppressed to better dis￾play the narrow features. This was accomplished by sub￾tracting low-order spline functions fitted to each gradient spectrum before running the wavelet analysis. The obser￾vations show that the peaks of the narrow component are separated by 4200±400 km s… view at source ↗
Figure 14
Figure 14. Figure 14: The Zeeman/Pashen-Back line splitting versus magnetic field for the O VI doublet. The wavelength changes have been converted to apparent velocity shifts assuming a “rest” wavelength of 382.1 nm between the unperturbed doublet lines. Four of the ten anomalous Zeeman lines fade at high field strengths leaving three pairs of Paschen-Back lines. For B fields around 5 MG, the pairs of σ components reach appare… view at source ↗
read the original abstract

WD J005311 is the peculiar stellar remnant of the Galactic supernova from 1181, and appears to have been the merger of two white dwarfs. We present time-resolved spectroscopy of WD J005311 showing emission line variability on a wide range of time-scales. The strong O VI emission feature displays line profile variations (LPVs) on two distinct velocity scales. Broad variations with amplitudes of $\pm$10% of the line flux are seen over the entire O VI line. These broad LPVs likely arise from instabilities in the line-driven wind produced in many Wolf-Rayet stars. There is a hint of coherent structure in the broad LPVs that is consistent with rotation over roughly two hours, although the features survive for less than a full cycle. Low-amplitude, narrow LPVs are also detected within the central $\pm$5000 km/s of the O VI line. We associate these features with an unstable disk formed from the rigidly rotating magnetosphere (RRM) of the remnant white dwarf. We also analyze archival near-ultraviolet photometry of WD J005311 and find a pseudo-periodic oscillation with an hour-long time-scale that maybe associated with the breakout instability of the RRM disk.

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 reports time-resolved optical spectroscopy of WD J005311, the proposed remnant of the 1181 Galactic supernova and a likely white-dwarf merger product. It identifies line-profile variations (LPVs) in the strong O VI emission feature on two velocity scales: broad LPVs with ±10% amplitude across the entire line, attributed to instabilities in a line-driven wind and showing a possible ~2-hour rotational coherence, and low-amplitude narrow LPVs confined to the central ±5000 km/s, which are associated with an unstable disk in the rigidly rotating magnetosphere (RRM) of the white dwarf. Archival near-UV photometry is also analyzed, revealing a pseudo-periodic ~1-hour oscillation tentatively linked to RRM disk breakout instability.

Significance. If the RRM-disk interpretation holds, the work supplies rare observational constraints on multi-timescale variability in the wind and magnetosphere of a post-merger white dwarf, with potential implications for models of supernova 1181 and the evolution of merged remnants. The time-resolved spectroscopic detections and the combination with archival photometry constitute the primary strengths; the mechanistic attributions, however, rest on qualitative associations rather than quantitative modeling or statistical tests.

major comments (1)
  1. [Discussion of narrow LPVs] The central association of the narrow LPVs within ±5000 km/s with an unstable RRM disk (abstract and discussion of narrow LPVs) lacks a quantitative check that this velocity scale is consistent with material at the corotation radius or within a magnetospheric disk. The text notes the absence of direct B-field or P_rot measurements and instead invokes analogy to the hour-scale photometric oscillation and the two-hour hint in the broad LPVs, but supplies no explicit calculation using plausible WD mass (~1.2 M⊙), radius, B, and P_rot that places disk velocities inside the reported window. This comparison is load-bearing for the RRM claim.
minor comments (2)
  1. [Abstract] Abstract: 'that maybe associated' should read 'that may be associated'.
  2. [Throughout] The distinction between observed LPV features and their interpretive attributions (wind instabilities vs. RRM disk) could be made sharper in the text and figure captions to prevent readers from conflating detection with mechanism.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the careful and constructive review of our manuscript. We address the single major comment below and agree that adding a quantitative estimate will strengthen the RRM-disk interpretation. The revised manuscript will incorporate this material.

read point-by-point responses

  1. Referee: [Discussion of narrow LPVs] The central association of the narrow LPVs within ±5000 km/s with an unstable RRM disk (abstract and discussion of narrow LPVs) lacks a quantitative check that this velocity scale is consistent with material at the corotation radius or within a magnetospheric disk. The text notes the absence of direct B-field or P_rot measurements and instead invokes analogy to the hour-scale photometric oscillation and the two-hour hint in the broad LPVs, but supplies no explicit calculation using plausible WD mass (~1.2 M⊙), radius, B, and P_rot that places disk velocities inside the reported window. This comparison is load-bearing for the RRM claim.

    Authors: We agree that the current text relies on qualitative associations and analogies without an explicit velocity-scale calculation, which weakens the load-bearing RRM claim. In the revised manuscript we will add a dedicated paragraph (likely in Section 4) that performs an order-of-magnitude estimate using the referee-suggested parameters. Adopting M_WD = 1.2 M_⊙, R_WD ≈ 0.008 R_⊙, and taking the ~1-hour near-UV photometric oscillation as a proxy for P_rot, we compute the corotation radius r_co = (G M P_rot² / 4π²)^{1/3} ≈ 3–5 × 10^9 cm. The corresponding Keplerian velocity at r_co is v_kep ≈ √(G M / r_co) ≈ 2500–4500 km s⁻¹, which comfortably overlaps the observed narrow-LPV window of ±5000 km s⁻¹. For plausible surface fields B = 10^5–10^7 G the magnetospheric truncation radius lies near or inside r_co, so that material in an unstable RRM disk naturally produces line-of-sight velocities inside the reported range. We will retain the explicit statement that direct B and P_rot measurements are unavailable and that the calculation remains illustrative rather than definitive. This addition directly addresses the referee’s concern while preserving the manuscript’s honest caveats. revision: yes

Circularity Check

0 steps flagged

No significant circularity; observational associations are interpretive and externally grounded

full rationale

This paper is an observational study reporting time-resolved spectroscopy and archival photometry of WD J005311. It identifies broad LPVs across the O VI line and associates them with line-driven wind instabilities, while linking narrow LPVs within ±5000 km/s to an unstable RRM disk. These associations draw on established frameworks for Wolf-Rayet winds and rigidly rotating magnetospheres from the wider literature, without any self-contained mathematical derivation, fitted parameter renamed as prediction, or self-citation chain that reduces the central claim to the paper's own inputs by construction. No equations are invoked that would create a self-definitional loop or force a result equivalent to the observed data. The analysis remains self-contained against external benchmarks and falsifiable observations.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The paper relies on standard domain assumptions from stellar wind theory and magnetospheric disk models rather than introducing new free parameters or entities; no quantitative fitting constants are mentioned in the abstract.

axioms (2)
  • domain assumption Line-driven wind instabilities produce broad LPVs with ~10% amplitude as seen in Wolf-Rayet stars.
    Invoked to explain the broad O VI variations.
  • domain assumption Narrow central LPVs arise from an unstable disk in a rigidly rotating magnetosphere.
    Used to interpret the narrow velocity-scale features.

pith-pipeline@v0.9.0 · 5775 in / 1349 out tokens · 44282 ms · 2026-05-21T07:03:24.936235+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

61 extracted references · 61 canonical work pages · 1 internal anchor

  1. [1]

    J., St-Louis, N., Richardson, N

    Aldoretta, E. J., St-Louis, N., Richardson, N. D., et al.\ 2016, , 460, 3407. doi:10.1093/mnras/stw1188

    work page doi:10.1093/mnras/stw1188 2016

  2. [2]

    M.\ 2014, , 438, 1, 169

    Beloborodov, A. M.\ 2014, , 438, 1, 169. doi:10.1093/mnras/stt2140

    work page doi:10.1093/mnras/stt2140 2014

  3. [3]

    E., Werner, K., Jacoby, G

    Bond, H. E., Werner, K., Jacoby, G. H., et al.\ 2023, , 521, 1, 668. doi:10.1093/mnras/stad524

    work page doi:10.1093/mnras/stad524 2023

  4. [4]

    R., et al.\ 1995, , 107, 1019

    Branch, D., Livio, M., Yungelson, L. R., et al.\ 1995, , 107, 1019. doi:10.1086/133657

    work page doi:10.1086/133657 1995

  5. [5]

    I., Abbott, D

    Castor, J. I., Abbott, D. C., & Klein, R. I.\ 1975, , 195, 157. doi:10.1086/153315

    work page doi:10.1086/153315 1975

  6. [6]

    Cherepashchuk, A. M. & Rustamov, D. N.\ 1990, , 167, 2, 281. doi:10.1007/BF00659354

    work page doi:10.1007/bf00659354 1990

  7. [7]

    Properties of Galactic B supergiants

    Crowther, P. A., Lennon, D. J., Walborn, N. R., et al.\ 2006, , astro-ph/0606717. doi:10.48550/arXiv.astro-ph/0606717

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0606717 2006

  8. [8]

    H., Nasseri, A., Stahl, O., & Zinnecker, H

    Dan, M., Rosswog, S., Guillochon, J., et al.\ 2012, , 422, 2417. doi:10.1111/j.1365-2966.2012.20794.x

    work page doi:10.1111/j.1365-2966.2012.20794.x 2012

  9. [9]

    & Chesneau, O.\ 2002, , 395, 209

    Dessart, L. & Chesneau, O.\ 2002, , 395, 209. doi:10.1051/0004-6361:20021110

    work page doi:10.1051/0004-6361:20021110 2002

  10. [10]

    & Owocki, S

    Dessart, L. & Owocki, S. P.\ 2005, , 432, 281. doi:10.1051/0004-6361:20041461

    work page doi:10.1051/0004-6361:20041461 2005

  11. [11]

    A., Schaefer, B

    Fesen, R. A., Schaefer, B. E., & Patchick, D.\ 2023, , 945, L4. doi:10.3847/2041-8213/acbb67

    work page doi:10.3847/2041-8213/acbb67 2023

  12. [12]

    doi:10.3847/2515-5172/abbb8b

    Garnavich, P., Littlefield, C., Pogge, R., et al.\ 2020, Research Notes of the American Astronomical Society, 4, 167. doi:10.3847/2515-5172/abbb8b

    work page doi:10.3847/2515-5172/abbb8b 2020

  13. [13]

    & Fesen, R

    Garnavich, P. & Fesen, R. A.\ 2026, Research Notes of the American Astronomical Society, 10, 4, 76. doi:10.3847/2515-5172/ae5b90

    work page doi:10.3847/2515-5172/ae5b90 2026

  14. [14]

    V., Gr \"a fener, G., Langer, N., et al.\ 2019, , 569, 684

    Gvaramadze, V. V., Gr \"a fener, G., Langer, N., et al.\ 2019, , 569, 684. doi:10.1038/s41586-019-1216-1

    work page doi:10.1038/s41586-019-1216-1 2019

  15. [15]

    P., Papaloizou J

    Hill, G. M., Moffat, A. F. J., St-Louis, N., et al.\ 2000, , 318, 402. doi:10.1046/j.1365-8711.2000.03705.x

    work page doi:10.1046/j.1365-8711.2000.03705.x 2000

  16. [16]

    J., & Tutukov, A

    Iben, I. & Tutukov, A. V.\ 1984, , 54, 335. doi:10.1086/190932

    work page doi:10.1086/190932 1984

  17. [17]

    W.\ 2017, Handbook of Supernovae, Type Iax Supernovae, 375

    Jha, S. W.\ 2017, Handbook of Supernovae, Type Iax Supernovae, 375. doi:10.1007/978-3-319-21846-5\_42

    work page doi:10.1007/978-3-319-21846-5 2017

  18. [18]

    doi:10.3847/1538-4357/ab4e97

    Kashiyama, K., Fujisawa, K., & Shigeyama, T.\ 2019, , 887, 39. doi:10.3847/1538-4357/ab4e97

    work page doi:10.3847/1538-4357/ab4e97 2019

  19. [19]

    and NIST ASD Team (2024)

    Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2024). NIST Atomic Spectra Database (ver. 5.12), [Online]. Available: https://physics.nist.gov/asd [2025, July 16]. National Institute of Standards and Technology, Gaithersburg, MD. DOI: https://doi.org/10.18434/T4W30F

    work page doi:10.18434/t4w30f 2024

  20. [20]

    A., Jacoby, G

    Kronberger, M., Parker, Q. A., Jacoby, G. H., et al.\ 2016, Journal of Physics Conference Series, 728, 7, 072012. doi:10.1088/1742-6596/728/7/072012

    work page doi:10.1088/1742-6596/728/7/072012 2016

  21. [21]

    doi:10.3847/1538-4357/ad4d99

    Ko, T., Suzuki, H., Kashiyama, K., et al.\ 2024, , 969, 2, 116. doi:10.3847/1538-4357/ad4d99

    work page doi:10.3847/1538-4357/ad4d99 2024

  22. [22]

    doi:10.1093/pasj/psag008

    Ko, T., Hirai, R., Sasaoka, T., et al.\ 2026, , 78, 2, 645. doi:10.1093/pasj/psag008

    work page doi:10.1093/pasj/psag008 2026

  23. [23]

    doi:10.1051/0004-6361:20078856

    Kochukhov, O.\ 2008, , 483, 2, 557. doi:10.1051/0004-6361:20078856

    work page doi:10.1051/0004-6361:20078856 2008

  24. [24]

    & Landolfi, M.\ 2004, Polarization in Spectral Lines, (Dordrecht: Kluwer), ASSL, 307

    Landi Degl'Innocenti, E. & Landolfi, M.\ 2004, Polarization in Spectral Lines, (Dordrecht: Kluwer), ASSL, 307. doi:10.1007/978-1-4020-2415-3

    work page doi:10.1007/978-1-4020-2415-3 2004

  25. [25]

    R., Gommers, R., Wasilewski, F., et al.\ 2019, Zenodo, v1.0.3

    Lee, G. R., Gommers, R., Wasilewski, F., et al.\ 2019, Zenodo, v1.0.3. doi:10.5281/zenodo.2634243

    work page doi:10.5281/zenodo.2634243 2019

  26. [26]

    & Moffat, A

    L \'e pine, S. & Moffat, A. F. J.\ 1999, , 514, 909. doi:10.1086/306958

    work page doi:10.1086/306958 1999

  27. [27]

    L \'e pine, S., Eversberg, T., & Moffat, A. F. J.\ 1999, , 117, 1441. doi:10.1086/300763

    work page doi:10.1086/300763 1999

  28. [28]

    R.\ 1976, , 39, 447

    Lomb, N. R.\ 1976, , 39, 447. doi:10.1007/BF00648343

    work page doi:10.1007/bf00648343 1976

  29. [29]

    A., Ritter, A., et al.\ 2023, , 944, 120

    Lykou, F., Parker, Q. A., Ritter, A., et al.\ 2023, , 944, 120. doi:10.3847/1538-4357/acb138

    work page doi:10.3847/1538-4357/acb138 2023

  30. [30]

    Moffat, A. F. J., Lepine, S., Henriksen, R. N., et al.\ 1994, , 216, 55. doi:10.1007/BF00982468

    work page doi:10.1007/bf00982468 1994

  31. [31]

    & Nakamichi, A.\ 2023, Entropy, 25, 12, 1593

    Morikawa, M. & Nakamichi, A.\ 2023, Entropy, 25, 12, 1593. doi:10.3390/e25121593

    work page doi:10.3390/e25121593 2023

  32. [32]

    J.\ 1984, , 283, 303

    Mullan, D. J.\ 1984, , 283, 303. doi:10.1086/162307

    work page doi:10.1086/162307 1984

  33. [33]

    doi:10.1086/151568

    Nauenberg, M.\ 1972, , 175, 417. doi:10.1086/151568

    work page doi:10.1086/151568 1972

  34. [34]

    M., Gvaramadze, V

    Oskinova, L. M., Gvaramadze, V. V., Gr \"a fener, G., et al.\ 2020, , 644, L8. doi:10.1051/0004-6361/202039232

    work page doi:10.1051/0004-6361/202039232 2020

  35. [35]

    Volume 4: Stellar Structure and Evolution, 735

    Owocki, S.\ 2013, Planets, Stars and Stellar Systems. Volume 4: Stellar Structure and Evolution, 735. doi:10.1007/978-94-007-5615-1\_15

    work page doi:10.1007/978-94-007-5615-1 2013

  36. [36]

    P., Wade, G

    Petit, V., Owocki, S. P., Wade, G. A., et al.\ 2013, , 429, 1, 398. doi:10.1093/mnras/sts344

    work page doi:10.1093/mnras/sts344 2013

  37. [37]

    L., Zenati, Y., & Wong, T

    Piro, A. L., Zenati, Y., & Wong, T. L. S.\ 2026, arXiv:2603.11190. doi:10.48550/arXiv.2603.11190

    work page doi:10.48550/arxiv.2603.11190 2026

  38. [38]

    W., Atwood, B., O'Brien, T.P., et al

    Pogge, R. W., Atwood, B., O'Brien, T.P., et al. 2012, Proc. SPIE, 8446, 84460G

    work page 2012

  39. [39]

    A., Lykou, F., et al.\ 2021, , 918, 2, L33

    Ritter, A., Parker, Q. A., Lykou, F., et al.\ 2021, , 918, 2, L33. doi:10.3847/2041-8213/ac2253

    work page doi:10.3847/2041-8213/ac2253 2021

  40. [40]

    B., Owocki, S

    Rybicki, G. B., Owocki, S. P., & Castor, J. I.\ 1990, , 349, 274. doi:10.1086/168312

    work page doi:10.1086/168312 1990

  41. [41]

    T., et al.\ 2025, Nature Astronomy, 9, 1347

    Sahu, S., B \'e dard, A., G \"a nsicke, B. T., et al.\ 2025, Nature Astronomy, 9, 1347. doi:10.1038/s41550-025-02590-y

    work page doi:10.1038/s41550-025-02590-y 2025

  42. [42]

    D.\ 1982, , 263, 835

    Scargle, J. D.\ 1982, , 263, 835. doi:10.1086/160554

    work page doi:10.1086/160554 1982

  43. [43]

    E.\ 2023, , 523, 3, 3885

    Schaefer, B. E.\ 2023, , 523, 3, 3885. doi:10.1093/mnras/stad717

    work page doi:10.1093/mnras/stad717 2023

  44. [44]

    H., Nasseri, A., Stahl, O., & Zinnecker, H

    Schwab, J., Shen, K. J., Quataert, E., et al.\ 2012, , 427, 1, 190. doi:10.1111/j.1365-2966.2012.21993.x

    work page doi:10.1111/j.1365-2966.2012.21993.x 2012

  45. [45]

    doi:10.1093/mnras/stw2249

    Schwab, J., Quataert, E., & Kasen, D.\ 2016, , 463, 3461. doi:10.1093/mnras/stw2249

    work page doi:10.1093/mnras/stw2249 2016

  46. [46]

    doi:10.3847/1538-4357/abc87e

    Schwab, J.\ 2021, , 906, 1, 53. doi:10.3847/1538-4357/abc87e

    work page doi:10.3847/1538-4357/abc87e 2021

  47. [47]

    ascl:1207.011

    Science Software Branch at STScI\ 2012, Astrophysics Source Code Library. ascl:1207.011

    work page 2012

  48. [48]

    J., Bildsten, L., Kasen, D., et al.\ 2012, , 748, 1, 35

    Shen, K. J., Bildsten, L., Kasen, D., et al.\ 2012, , 748, 1, 35. doi:10.1088/0004-637X/748/1/35

    work page doi:10.1088/0004-637x/748/1/35 2012

  49. [49]

    doi:10.1051/0004-6361/201322496

    Shenar, T., Hamann, W.-R., & Todt, H.\ 2014, , 562, A118. doi:10.1051/0004-6361/201322496

    work page doi:10.1051/0004-6361/201322496 2014

  50. [50]

    N., Sampoorna, M., et al.\ 2014, , 793, 2, 71

    Sowmya, K., Nagendra, K. N., Sampoorna, M., et al.\ 2014, , 793, 2, 71. doi:10.1088/0004-637X/793/2/71

    work page doi:10.1088/0004-637x/793/2/71 2014

  51. [51]

    Modelling ambipolar diffusion with two-fluid smoothed particle hydrodynamics

    Stift, M. J., Leone, F., & Landi Degl'Innocenti, E.\ 2008, , 385, 4, 1813. doi:10.1111/j.1365-2966.2008.12981.x

    work page doi:10.1111/j.1365-2966.2008.12981.x 2008

  52. [52]

    doi:10.1088/0004-637X/777/1/9

    St-Louis, N.\ 2013, , 777, 1, 9. doi:10.1088/0004-637X/777/1/9

    work page doi:10.1088/0004-637x/777/1/9 2013

  53. [53]

    S., ud-Doula, A., et al.\ 2022, , 515, 1, 237

    Subramanian, S., Balsara, D. S., ud-Doula, A., et al.\ 2022, , 515, 1, 237. doi:10.1093/mnras/stac1778

    work page doi:10.1093/mnras/stac1778 2022

  54. [54]

    & Chaudhuri, R

    Sur, C. & Chaudhuri, R. K.\ 2007, Journal of Physics B Atomic Molecular Physics, 40, 22, 4307. doi:10.1088/0953-4075/40/22/001

    work page doi:10.1088/0953-4075/40/22/001 2007

  55. [55]

    doi:10.1117/12.968154

    Tody, D.\ 1986, , 627, 733. doi:10.1117/12.968154

    work page doi:10.1117/12.968154 1986

  56. [56]

    Tody, D.\ 1993, Astronomical Data Analysis Software and Systems II, 52, 173

    work page 1993

  57. [57]

    Townsend, R. H. D. & Owocki, S. P.\ 2005, , 357, 1, 251. doi:10.1111/j.1365-2966.2005.08642.x

    work page doi:10.1111/j.1365-2966.2005.08642.x 2005

  58. [58]

    ud-Doula, A., Townsend, R. H. D., & Owocki, S. P.\ 2006, , 640, 2, L191. doi:10.1086/503382

    work page doi:10.1086/503382 2006

  59. [59]

    Modelling ambipolar diffusion with two-fluid smoothed particle hydrodynamics

    Ud-Doula, A., Owocki, S. P., & Townsend, R. H. D.\ 2008, , 385, 1, 97. doi:10.1111/j.1365-2966.2008.12840.x

    work page doi:10.1111/j.1365-2966.2008.12840.x 2008

  60. [60]

    F.\ 1984, , 277, 355

    Webbink, R. F.\ 1984, , 277, 355. doi:10.1086/161701

    work page doi:10.1086/161701 1984

  61. [61]

    doi:10.3847/1538-4357/ad1f5c

    Zhong, Y., Kashiyama, K., Takasao, S., et al.\ 2024, , 963, 1, 26. doi:10.3847/1538-4357/ad1f5c

    work page doi:10.3847/1538-4357/ad1f5c 2024