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arxiv: 2606.25515 · v1 · pith:BL5AR4P2new · submitted 2026-06-24 · 🌌 astro-ph.HE

Accreting Compact Object Binaries with the SKA

Aru Beri , Francesco Carotenuto , Rob P. Fender , James C.A. Miller-Jones , Sara Motta , Valeriu Tudose , Jakob van den Eijnden This is my paper

Pith reviewed 2026-06-25 20:58 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords accreting binariescompact objectsSKArelativistic jetsblack hole X-ray binariesneutron starswhite dwarfsaccretion-ejection coupling
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The pith

The SKA will extend jet and accretion studies from bright black hole binaries to fainter neutron star and white dwarf systems plus nearby galaxies.

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

Accreting compact object binaries let observers watch how matter falls in and launches jets on human timescales, with patterns that scale across stellar-mass to supermassive objects. The paper claims the SKA's gains in point-source sensitivity, surface-brightness sensitivity, angular resolution, and frequency coverage will open these processes to populations now too faint or distant to study in detail. This means moving from existing black-hole work to neutron-star and white-dwarf accretors, uncovering hidden quiescent systems, and reaching rare high-accretion phases in external galaxies.

Core claim

Accreting binary systems provide a time-resolved view of the accretion and ejection processes that are seen in all classes of compact objects, from stellar-mass to supermassive. They allow us to study the launching of relativistic jets on human timescales, probing how the jets are coupled to the underlying accretion flow, and providing unique insights that can be extended to supermassive black holes via the well-established mass scale invariance. The SKA will enhance such studies via its high point source and surface brightness sensitivity, high angular resolution, and broad frequency coverage. This will enable the extension of our existing black hole studies to the fainter accreting neutron

What carries the argument

The SKA's high point-source sensitivity, surface-brightness sensitivity, angular resolution, and broad frequency coverage applied to radio emission from jets in accreting binaries.

If this is right

  • Jet-launching studies can now include the effects of stellar surfaces and magnetic fields in neutron stars and white dwarfs.
  • A more complete census of Galactic black holes becomes possible through detection of their quiescent, low-luminosity states.
  • Rare high-accretion-rate phases that trace black-hole growth can be observed directly in nearby galaxies.
  • Comparative samples across compact-object types will test how mass, spin, and magnetic field strength control jet power.
  • Feedback from jets into the interstellar medium can be quantified for a wider range of source luminosities.

Where Pith is reading between the lines

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

  • Successful SKA observations would strengthen the mass-scaling argument that links stellar-mass jet physics to active galactic nuclei.
  • Detection of many new quiescent systems could revise estimates of the total number and evolutionary lifetimes of compact-object binaries.
  • Broad frequency coverage may allow spectral decomposition of jet emission that is currently blended in lower-sensitivity data.
  • The same sensitivity leap could be used to search for radio counterparts to gravitational-wave events involving compact objects.

Load-bearing premise

The SKA will reach its planned sensitivity, resolution, and frequency performance, and that jet-accretion coupling relations measured in bright black holes will continue to hold for much fainter neutron-star, white-dwarf, and extragalactic systems.

What would settle it

After SKA operations begin, no new population of faint accreting neutron-star or white-dwarf binaries is detected in the Galactic plane or Magellanic Clouds, and no resolved jets appear in any nearby galaxy despite the predicted sensitivity gain.

Figures

Figures reproduced from arXiv: 2606.25515 by Aru Beri, Francesco Carotenuto, Jakob van den Eijnden, James C.A. Miller-Jones, Rob P. Fender, Sara Motta, Valeriu Tudose.

Figure 1
Figure 1. Figure 1: Radio/X-ray luminosity plane, showing the measured positions of a sample of black hole and neu￾tron star X-ray binaries, indicating the (unshaded) region accessible to SKA-VLBI astrometric observations (detection threshold 10 𝜇Jy) for a source at 4 kpc (Bahramian and Rushton, 2022). 8 Comparing Black Holes and Neutron Stars: Dissecting the Physics of Jet Launching The SKA will revolutionize comparative jet… view at source ↗
read the original abstract

Accreting binary systems provide a time-resolved view of the accretion and ejection processes that are seen in all classes of compact objects, from stellar-mass to supermassive. They allow us to study the launching of relativistic jets on human timescales, probing how the jets are coupled to the underlying accretion flow, and providing unique insights that can be extended to supermassive black holes via the well-established mass scale invariance. Comparative studies of jets from different classes of compact objects allow us to determine the impact of mass, spin, magnetic fields, and stellar surfaces on the launching of jets. The jets from black hole X-ray binaries provide probes of the Galactic black hole population, and an important source of feedback to the surrounding interstellar medium. While existing radio facilities (including the SKA precursors) have made great progress in this field in recent years, the SKA will enhance such studies via its high point source and surface brightness sensitivity, high angular resolution, and broad frequency coverage. This will enable the extension of our existing black hole studies to the fainter accreting neutron star and white dwarf population, the detection of previously-undiscovered systems in a low-luminosity quiescent state, and the extension of our studies to nearby galaxies, revealing rare, high-accretion rate systems that probe a key phase of black hole growth.

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

0 major / 1 minor

Summary. The manuscript presents a forward-looking science case for using the Square Kilometre Array (SKA) to study accreting compact object binaries. It reviews how these systems provide time-resolved views of accretion-jet coupling across stellar-mass to supermassive scales, and argues that the SKA's point-source and surface-brightness sensitivity, angular resolution, and frequency coverage will extend existing black-hole X-ray binary work to fainter neutron-star and white-dwarf populations, enable detection of quiescent systems, and permit studies in nearby galaxies.

Significance. If the projected SKA performance specifications are realized, the paper supplies a useful roadmap for comparative jet studies and for probing rare high-accretion phases of black-hole growth. The arguments rest on established mass-scaling relations and standard assumptions about instrument performance rather than new derivations or data.

minor comments (1)
  1. [Abstract] Abstract, final paragraph: the claim that SKA will enable extension to nearby galaxies would be strengthened by a brief, explicit citation to the relevant SKA design sensitivity or resolution figures that support the extragalactic reach.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their supportive summary and recommendation of minor revision. The review correctly identifies the manuscript as a forward-looking perspective paper that relies on established scaling relations and instrument projections rather than new derivations.

Circularity Check

0 steps flagged

No significant circularity in this science case review

full rationale

This is a forward-looking perspective paper outlining a science case for SKA observations of accreting binaries. It contains no derivations, equations, fitted parameters, model predictions, or uniqueness theorems. All statements about SKA capabilities and extensions to neutron star/white dwarf populations or nearby galaxies are prospective applications of established accretion-jet scaling relations and instrument specifications, with no self-referential reduction, self-citation load-bearing, or renaming of results. The text is self-contained against external benchmarks of radio astronomy capabilities and does not invoke any internal consistency checks that loop back to its own inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No free parameters, axioms, or invented entities are introduced; the paper is a review of anticipated observational capabilities without derivations or new postulates.

pith-pipeline@v0.9.1-grok · 5791 in / 1039 out tokens · 15568 ms · 2026-06-25T20:58:35.567655+00:00 · methodology

discussion (0)

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Works this paper leans on

76 extracted references · 75 canonical work pages

  1. [2]

    doi: 10.1038/s41586-024-07995-9. T. An et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1038/s41586-024-07995-9

  2. [3]

    doi: 10.1093/mnras/stz2335. P. Atri et al.A&A, 696:A223, Apr

    work page doi:10.1093/mnras/stz2335

  3. [4]

    doi: 10.1051/0004-6361/202452837. M. Bachetti et al.Nature, 514(7521):202–204, Oct

    work page doi:10.1051/0004-6361/202452837

  4. [5]

    doi: 10.1038/nature13791. A. Bahramian and A. Rushton. bersavosh/xrb-lrlx_pub: update 20220908. doi: 10.5281/zen- odo.7059313, Sept

    work page doi:10.1038/nature13791

  5. [6]

    T.M.Belloni

    doi: 10.3847/2041-8213/accde1. T.M.Belloni. StatesandTransitionsinBlackHoleBinaries. InT.Belloni,editor,LectureNotesin Physics,BerlinSpringerVerlag,volume794,page53.2010.doi: 10.1007/978-3-540-76937-8_3. C. F. Bradshaw, E. B. Fomalont, and B. J. Geldzahler.ApJL, 512(2):L121–L124, Feb

    work page doi:10.3847/2041-8213/accde1 2041

  6. [7]

    doi: 10.1086/311889. J. Bright et al.Nature Astronomy, 4:1–7, 07

    work page doi:10.1086/311889

  7. [8]

    doi: 10.1038/s41550-020-1023-5. F. Carotenuto et al.MNRAS, 504(1):444–468, June

    work page doi:10.1038/s41550-020-1023-5

  8. [9]

    doi: 10.1093/mnras/stab864. F. Carotenuto et al.MNRAS, 533(4):4188–4209, Oct

    work page doi:10.1093/mnras/stab864

  9. [10]

    doi: 10.1093/mnras/stae2049. S. Carpano, F. Haberl, C. Maitra, and G. Vasilopoulos.MNRAS, 476(1):L45–L49, feb

    work page doi:10.1093/mnras/stae2049

  10. [11]

    doi: 10.1093/mnrasl/sly030. L. Chomiuk et al.ApJ, 777(1):69, Nov

    work page doi:10.1093/mnrasl/sly030

  11. [12]

    doi: 10.1088/0004-637X/777/1/69. K. Choudhury, J. A. García, J. F. Steiner, and C. Bambi.ApJ, 851(1):57, Dec

    work page doi:10.1088/0004-637x/777/1/69

  12. [13]

    doi: 10.3847/1538-4357/aa9925. E. J. M. Colbert and R. F. Mushotzky.ApJ, 519(1):89–107, July

    work page doi:10.3847/1538-4357/aa9925

  13. [14]

    doi: 10.1086/307356. A. J. Cooper et al.MNRAS, July

    work page doi:10.1086/307356

  14. [15]

    doi: 10.1093/mnras/staf1085. D. L. Coppejans et al.MNRAS, 451(4):3801–3813, Aug

    work page doi:10.1093/mnras/staf1085

  15. [16]

    doi: 10.1093/mnras/stv1225. D. L. Coppejans et al.MNRAS, 463(2):2229–2241, Dec

    work page doi:10.1093/mnras/stv1225

  16. [17]

    doi: 10.1093/mnras/stw2133. M. Coriat et al.MNRAS, 414(1):677–690, June

    work page doi:10.1093/mnras/stw2133

  17. [18]

    doi: 10.1111/j.1365-2966.2011.18433.x. J. M. Corral-Santana et al.A&A, 587:A61, Mar

    work page doi:10.1111/j.1365-2966.2011.18433.x 2011

  18. [19]

    doi: 10.1051/0004-6361/201527130. D. Cseh et al.MNRAS, 439(1):L1–L5, 01

    work page doi:10.1051/0004-6361/201527130

  19. [20]

    doi: 10.1093/mnrasl/slt166. P. Das and O. Porth.ApJL, 960(2):L12, Jan

    work page doi:10.1093/mnrasl/slt166

  20. [21]

    doi: 10.3847/2041-8213/ad151f. A.-J. Dong, Q. Wu, and X.-F. Cao.ApJL, 787(2):L20, June

    work page doi:10.3847/2041-8213/ad151f 2041

  21. [22]

    doi: 10.1088/2041-8205/787/2/ L20. K. El-Badry et al.MNRAS, 521(3):4323–4348, May 2023a. doi: 10.1093/mnras/stad799. K. El-Badry et al.MNRAS, 518(1):1057–1085, Jan. 2023b. doi: 10.1093/mnras/stac3140. EventHorizonTelescopeCollaborationetal.ApJL,875(1):L1,Apr.2019.doi: 10.3847/2041-8213/ ab0ec7. S. Fabrika et al.Nature Physics, 11(7):551–553, July

    work page doi:10.1088/2041-8205/787/2/ 2041

  22. [23]

    13 Accreting Compact Object Binaries with the SKA A

    doi: 10.1038/nphys3348. 13 Accreting Compact Object Binaries with the SKA A. Beri et al. R. Fender and J. Bright.MNRAS, 489(4):4836–4846, Nov

    work page doi:10.1038/nphys3348

  23. [24]

    doi: 10.1093/mnras/stz2000. R. Fender and T. Muñoz-Darias. The Balance of Power: Accretion and Feedback in Stellar Mass BlackHoles. InF.Haardtetal.,editors,LectureNotesinPhysics,BerlinSpringerVerlag,volume 905, page

    work page doi:10.1093/mnras/stz2000

  24. [25]

    doi: 10.1007/978-3-319-19416-5_3. R. Fender et al.Astronomy and Geophysics, 64(6):6.24–6.30, Dec

    work page doi:10.1007/978-3-319-19416-5_3

  25. [26]

    doi: 10.1093/astrogeo/ atad059. R. P. Fender, T. M. Belloni, and E. Gallo.MNRAS, 355(4):1105–1118, Dec

    work page doi:10.1093/astrogeo/

  26. [27]

    2009, MNRAS, 394, 1825, doi:10.1111/j

    doi: 10.1111/j. 1365-2966.2004.08384.x. R. P. Fender, J. Bright, K. P. Mooley, and et al. InProceedings of Science (AASKA14), page 51,

    work page doi:10.1111/j 2004

  27. [28]

    Gaia Collaboration et al.A&A, 686:L2, June

    doi: 10.1088/0004-637X/697/2/1057. Gaia Collaboration et al.A&A, 686:L2, June

    work page doi:10.1088/0004-637x/697/2/1057

  28. [29]

    doi: 10.1051/0004-6361/202449763. E. Gallo, R. P. Fender, and G. G. Pooley.MNRAS, 344:60–72,

    work page doi:10.1051/0004-6361/202449763

  29. [30]

    Gallo et al.Nature, 436(7052):819–821, Aug

    E. Gallo et al.Nature, 436(7052):819–821, Aug. 2005a. doi: 10.1038/nature03879. E. Gallo, R. P. Fender, and R. I. Hynes.MNRAS, 356(3):1017–1021, Jan. 2005b. doi: 10.1111/j. 1365-2966.2004.08503.x. E. Gallo, R. P. Fender, J. C. A. Miller-Jones, and et al.MNRAS, 370:1351–1360,

    work page doi:10.1038/nature03879 2004

  30. [31]

    2012.21704.x

    E.Gallo,B.P.Miller,andR.Fender.MNRAS,423(1):590–599,052012. doi: 10.1111/j.1365-2966. 2012.20899.x. E. Gallo et al.MNRAS, 445(1):290–300, Nov

    work page doi:10.1111/j.1365-2966 2012

  31. [32]

    doi: 10.1093/mnras/stu1599. E. Gallo, N. Degenaar, and J. van den Eijnden.MNRAS, 478(1):L132–L136, July

    work page doi:10.1093/mnras/stu1599

  32. [33]

    doi: 10.1093/mnrasl/sly083. K. V. S. Gasealahwe et al.MNRAS, 541(4):4011–4024, Aug

    work page doi:10.1093/mnrasl/sly083

  33. [34]

    doi: 10.1093/mnras/staf1216. B. Giesers et al.MNRAS, 475(1):L15–L19, Mar

    work page doi:10.1093/mnras/staf1216

  34. [35]

    doi: 10.1093/mnrasl/slx203. B. Giesers et al.A&A, 632:A3, Dec

    work page doi:10.1093/mnrasl/slx203

  35. [36]

    doi: 10.1051/0004-6361/201936203. K. Gültekin et al.ApJ, 871(1):80, Jan

    work page doi:10.1051/0004-6361/201936203

  36. [37]

    doi: 10.3847/1538-4357/aaf6b9. J. F. Hao and S. N. Zhang.ApJ, 702(2):1648–1661, Sept

    work page doi:10.3847/1538-4357/aaf6b9

  37. [38]

    doi: 10.1088/0004-637X/702/2/

    work page doi:10.1088/0004-637x/702/2/

  38. [39]

    2003.06918.x

    doi: 10.1046/j.1365-8711. 2003.06918.x. G. L. Israel et al.Science, 355(6327):817–819, Feb. 2017a. doi: 10.1126/science.aai8635. G. L. Israel et al.MNRAS, 466(1):L48–L52, Mar. 2017b. doi: 10.1093/mnrasl/slw218. M.Janssenetal.NatureAstronomy,5:1017–1028,July2021. doi: 10.1038/s41550-021-01417-w. P. Kaaret, H. Feng, and T. P. Roberts.ARA&A, 55(1):303–341, Aug

    work page doi:10.1046/j.1365-8711 2003

  39. [40]

    doi: 10.1086/422466. A. King, J.-P. Lasota, and M. Middleton.New Astron. Rev., 96:101672, June

    work page doi:10.1086/422466

  40. [41]

    Hybrid bci for upper limb rehabilitation: integrating mi with peripheral field ssvep stimulation.Journal of Neuroscience Methods, 2025

    doi: 10.1016/j. newar.2022.101672. E. Körding et al.Science, 320(5881):1318, June

    work page doi:10.1016/j 2022

  41. [42]

    doi: 10.1126/science.1155492. C. Y. Lam et al.ApJL, 933(1):L23, July

    work page doi:10.1126/science.1155492

  42. [43]

    Lhaaso Collaboration et al.National Science Review, 12(12):nwaf496, Dec

    doi: 10.3847/2041-8213/ac7442. Lhaaso Collaboration et al.National Science Review, 12(12):nwaf496, Dec

    work page doi:10.3847/2041-8213/ac7442 2041

  43. [44]

    M.Longair.HighEnergyAstrophysics

    arXiv search: Report number AASKAII/Lin01. M.Longair.HighEnergyAstrophysics. CambridgeUniversityPress,2011. ISBN9781139494540. T.J.Maccarone. InAdvancingAstrophysicswiththeSquareKilometreArray(AASKA14),page85,

    2011

  44. [45]

    doi: 10.1002/asna.20230028. I. Mariani et al.A&A, 704:A239, Dec

    work page doi:10.1002/asna.20230028

  45. [46]

    doi: 10.1051/0004-6361/202556290. S. Markoff et al.A&A, 397:645–658, Jan

    work page doi:10.1051/0004-6361/202556290

  46. [47]

    doi: 10.1051/0004-6361:20021497. A. Merloni, S. Heinz, and T. di Matteo.MNRAS, 345(4):1057–1076, Nov

    work page doi:10.1051/0004-6361:20021497

  47. [48]

    1365-2966.2003.07017.x

    doi: 10.1046/j. 1365-2966.2003.07017.x. M. J. Middleton et al.Nature, 493(7431):187–190, Jan

    work page doi:10.1046/j 2003

  48. [49]

    doi: 10.1038/nature11697. S. Migliari and R. P. Fender.MNRAS, 366(1):79–91, Feb

    work page doi:10.1038/nature11697

  49. [50]

    doi: 10.1111/j.1365-2966.2005. 09777.x. J. M. Miller, A. C. Fabian, and M. C. Miller.ApJL, 614(2):L117–L120, Oct

    work page doi:10.1111/j.1365-2966.2005 2005

  50. [51]

    doi: 10.1111/j.1365-2966.2011. 20326.x. J. C. A. Miller-Jones et al.MNRAS, 453(4):3918–3931, Nov

    work page doi:10.1111/j.1365-2966.2011 2011

  51. [52]

    doi: 10.1093/mnras/stv1869. J. C. A. Miller-Jones et al.Science, 371(6533):1046–1049, Mar

    work page doi:10.1093/mnras/stv1869

  52. [53]

    doi: 10.1126/science. abb3363. I. F. Mirabel et al.Nature, 413(6852):139–141, Sept

    work page doi:10.1126/science

  53. [54]

    doi: 10.1038/35093060. C. Motch et al.Nature, 514(7521):198–201, Oct

    work page doi:10.1038/35093060

  54. [55]

    doi: 10.1038/nature13730. S. E. Motta et al.A&A, 696:A222, Apr

    work page doi:10.1038/nature13730

  55. [56]

    21 Transforming XRB Astrophysics with SKA+VLBI T

    doi: 10.1051/0004-6361/202452838. P.NagarajanandK.El-Badry.PASP,137(3):034203,Mar.2025. doi: 10.1088/1538-3873/adb6d6. R. Narayan and I. Yi.ApJ, 452:710, Oct

    work page doi:10.1051/0004-6361/202452838 2025

  56. [57]

    doi: 10.1086/176343. R. Narayan, I. V. Igumenshchev, and M. A. Abramowicz.PASJ, 55:L69–L72, Dec

    work page doi:10.1086/176343

  57. [58]

    doi: 10.1093/pasj/55.6.L69. M. W. Pakull, R. Soria, and C. Motch.Nature, 466(7303):209–212, July

    work page doi:10.1093/pasj/55.6.l69

  58. [59]

    doi: 10.3847/1538-4357/ad8b9c. K. Parfrey and A. Tchekhovskoy.ApJ, 975(1):57, Nov

    work page doi:10.3847/1538-4357/ad8b9c

  59. [60]

    doi: 10.3847/1538-4357/ad737b. R. M. Plotkin et al.MNRAS, 503(3):3784–3795, 03

    work page doi:10.3847/1538-4357/ad737b

  60. [61]

    doi: 10.1093/mnras/stab644. A. P. Rushton et al.MNRAS, 468(3):2788–2802, July

    work page doi:10.1093/mnras/stab644

  61. [62]

    doi: 10.1093/mnras/stx526. T. D. Russell et al.ApJ, 883(2):198, Oct

    work page doi:10.1093/mnras/stx526

  62. [63]

    doi: 10.3847/1538-4357/ab3d36. T. D. Russell et al.Nature, 627(8005):763–766, Mar

    work page doi:10.3847/1538-4357/ab3d36

  63. [64]

    doi: 10.1038/s41586-024-07133-5. K. C. Sahu et al.ApJ, 933(1):83, July

    work page doi:10.1038/s41586-024-07133-5

  64. [65]

    doi: 10.3847/1538-4357/ac739e. H. Sakemi et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.3847/1538-4357/ac739e

  65. [66]

    doi: 10.1093/mnrasl/slz086. N. I. Shakura and R. A. Sunyaev.A&A, 24:337–355, Jan

    work page doi:10.1093/mnrasl/slz086

  66. [67]

    J.F.SteinerandJ.E.McClintock.ApJ,745(2):136,Feb.2012.doi: 10.1088/0004-637X/745/2/136

    doi: 10.1093/mnrasl/slu183. J.F.SteinerandJ.E.McClintock.ApJ,745(2):136,Feb.2012.doi: 10.1088/0004-637X/745/2/136. J. Strader et al.Nature, 490(7418):71–73, Oct

    work page doi:10.1093/mnrasl/slu183 2012

  67. [68]

    doi: 10.1038/nature11490. A. Tchekhovskoy, R. Narayan, and J. C. McKinney.MNRAS, 418(1):L79–L83, Nov

    work page doi:10.1038/nature11490

  68. [69]

    doi: 10.1111/j.1745-3933.2011.01147.x. A. J. Tetarenko et al.MNRAS, 504(3):3862–3883, July

    work page doi:10.1111/j.1745-3933.2011.01147.x 2011

  69. [70]

    doi: 10.1093/mnras/stab820. J. van den Eijnden et al.MNRAS, 516(4):4844–4861, Nov

    work page doi:10.1093/mnras/stab820

  70. [71]

    doi: 10.1093/mnras/stac2518. X. Y. Wang, Z. G. Dai, and T. Lu.ApJ, 592(1):347–353, July

    work page doi:10.1093/mnras/stac2518

  71. [72]

    doi: 10.1086/375638. N. A. Webb et al.ApJL, 712:L107,

    work page doi:10.1086/375638

  72. [73]

    doi: 10.1088/2041-8205/712/1/L107. G. Wiktorowicz et al.ApJ, 885(1):1, Nov

    work page doi:10.1088/2041-8205/712/1/l107 2041

  73. [74]

    doi: 10.3847/1538-4357/ab45e6. B. Willems et al.ApJ, 625(1):324–346, May

    work page doi:10.3847/1538-4357/ab45e6

  74. [75]

    doi: 10.1086/429557. C. M. Wood et al.ApJL, 984(2):L53, May

    work page doi:10.1086/429557

  75. [76]

    doi: 10.3847/2041-8213/adc9b3. J. Yang et al.MNRAS, 526(1):L1–L7, 08

    work page doi:10.3847/2041-8213/adc9b3 2041

  76. [77]

    X.Zhangetal.arXive-prints,art.arXiv:2504.11945,Apr.2025

    doi: 10.1093/mnrasl/slad111. X.Zhangetal.arXive-prints,art.arXiv:2504.11945,Apr.2025. doi: 10.48550/arXiv.2504.11945. 16

    work page doi:10.1093/mnrasl/slad111 2025