Pith. sign in

REVIEW 1 cited by

Accretion of AGN Stars under Influence of Disk Geometry

T0 review · reviewed 2026-08-07 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read In cold, thin AGN disks, accretion onto embedded massive stars is capped by the smaller of the radiative critical radius and the Hill radius, about 0.02 solar masses per year in the simulated setup.

arxiv 2505.13951 v1 pith:N6SYDG6L submitted 2025-05-20 astro-ph.HE astro-ph.SR

Yi-Xian Chen , Yan-Fei Jiang , Jeremy Goodman This is my paper
classification astro-ph.HEastro-ph.SR
keywords accretiondiskbackgroundradiusstarswhenbecomescold
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Massive stars that form inside the disks around supermassive black holes are surrounded by gas. Earlier work assumed they pull gas in evenly from all directions. This paper replaces that assumption with a disk-shaped background: denser near the midplane, colder or hotter depending on temperature, and shearing past the star.

The simulations follow a 50-solar-mass star in a disk around a 100-million-solar-mass black hole. Five disk temperatures are tested. When the disk is hot and puffy, accretion stays roughly spherical and matches the old isotropic estimate. When the disk is cold and thin, the picture changes. Light from the star and the accreting gas escapes most easily in polar directions and drives outflows there, while the dense midplane keeps feeding gas inward. The effective size of the star's gravitational pull is no longer set by the usual sonic critical radius alone, but by the smaller of that radius and the Hill radius, giving rates of about 0.02 solar masses per year. The authors propose a simple formula: take the smaller of the two radii, square it, and multiply by the disk density and sound speed.

Most of the inflowing gas carries angular momentum, so the simulations also check what pushes angular momentum back out. They attribute it to spiral shocks generated by the black hole's tidal field, with an effective viscosity parameter between 0.1 and 1. The runs last only one orbital period, so long-term processes like gap-opening are not captured.

Extended reading notes

Core claim

The paper claims that when the background disk is cold and thin, accretion onto an embedded massive star becomes strongly anisotropic: super-Eddington outflows escape through the polar region while rapid accretion is sustained along the midplane, and the effective accretion cross-section is constrained by the Hill radius and disk scale height rather than the isotropic critical radius. It summarizes this in Equation 21: Mdot ~ 4*pi*rho0*cs,gas,0*min(R^2crit,iso, R^2Hill). If correct, the accretion rate for a 50-solar-mass star at rho ~ 1e-10 g/cm3 is capped near 0.02 solar masses per year over the 3 to 7 times 10^4 K temperature range.

Load-bearing premise

The entire analysis assumes the accretion flow is in the fast-diffusion regime, where radiation decouples from gas and acts as a reduction in gravity (Section 4.2). If the background density were roughly an order of magnitude higher, the diffusion time would exceed the dynamical time, accretion would become adiabatic, and the anisotropic radiative-feedback picture and the Hill-limited scaling in Equation 21 would no longer apply.

Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The paper introduces no new particles, forces, or conserved quantities. The free parameters are simulation inputs and one diagnostic fit; the central scaling relation has no additional fitted coefficient. The main assumptions are the fast-diffusion regime, the polytropic hydrostatic outer boundary, and the neglect of self-gravity, MRI/GI heating, and gap-opening.

free parameters (4)
  • Disk midplane density rho0 = 1e-10 g/cm3
    Fixed input boundary density used in all runs; the quoted accretion rates scale linearly with it in Equation 21. Chosen to represent an AGN disk midplane, not fitted to simulation output.
  • Disk midplane temperatures T0 = 3e4, 4e4, 5e4, 6e4, 7e4 K
    Chosen to span subthermal to superthermal regimes; the central regime-transition claim depends on these chosen values. Measured rates are reported without error bars.
  • Stellar and SMBH parameters = M_star = 50 Msun, M_bh = 1e8 Msun, r_bh = 0.001 pc
    Scenario inputs that fix the Hill radius and the background shear and tidal potentials. They are chosen, not fitted, but the central results depend on them.
  • Spiral pitch angle psi (diagnostic fit) = 53 degrees for run T3e4
    Fitted to the time-averaged midplane density snapshot in Appendix A to estimate alpha_wave; used only for the secondary spiral-shock angular-momentum transport argument.
assumptions (5)
  • domain assumption The background disk is in vertical hydrostatic equilibrium with P proportional to rho^(4/3), constant radiation-to-gas pressure ratio, and no disk self-gravity (Equation 3).
    Sets the outer boundary density and temperature profiles and the scale height; invoked in Section 2.1.
  • domain assumption Gas is fully ionized with mu = 0.60 m_p, X = 0.73, Y = 0.25, Z = 0.02, gamma = 5/3, and OPAL opacities.
    Standard composition and opacity choices for stellar envelopes and AGN disks, stated in Section 2.
  • domain assumption The accretion flow is in the fast-diffusion regime, so radiation decouples from gas and acts as reduced gravity.
    Explicitly scoped in Section 4.2; if the diffusion time exceeds the dynamical time, accretion becomes adiabatic and the anisotropic feedback picture and Equation 21 fail.
  • domain assumption The stellar envelope self-gravity is negligible; 99% of the stellar mass lies inside Rin = 24.65 Rsun and the inner boundary is fixed.
    Adopted from Section 2.1 following Chen et al. 2024; it would fail if an adiabatic self-gravitating envelope forms.
  • ad hoc to paper Local shearing-globe boundary conditions with fixed background profiles and no MRI or GI heating adequately represent the disk during the one-orbit integration.
    Acknowledged in Section 4.1; gap-opening, global torques, and turbulent heating are not modeled, so the long-term accretion rate may differ.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Accretion of AGN Stars under Influence of Disk Geometry." pith.science (2026). https://pith.science/paper/N6SYDG6L

@misc{pith2026250513951,
  author       = {Pith},
  title        = {Pith review of: Accretion of AGN Stars under Influence of Disk Geometry},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/N6SYDG6L}},
  note         = {Machine review of arXiv:2505.13951}
}
abstract

Massive stars can form within or be captured by AGN disks, influencing both the thermal structure and metallicity of the disk environment. In a previous work, we investigated isotropic accretion onto massive stars from a gas-rich, high-entropy background. Here, we consider a more realistic scenario by incorporating the stratified geometry of the background disk in our 3D radiation hydrodynamic simulatons. We find that accretion remains relatively isotropic when the disk is hot enough and the scale height is thicker than the accretion flow's nominal supersonic critical radius $R{crit}$ (sub-thermal). However, when the disk becomes cold, the accretion flow becomes significantly anisotropic (super-thermal). Escaping stellar and accretion luminosity can drive super-Eddington outflows in the polar region, while rapid accretion is sustained along the midplane. Eventually, the effective cross-section is constrained by the Hill radius and the disk scale height rather than the critical radius when the disk is cold enough. For our setup (stellar mass $\sim 50 M\odot$ and background density $\rho\sim 10^{-10}$ g/cm$^3$) the accretion rates is capped below $\sim 0.02M\odot$/year and the effective accretion parameter $\alpha\sim 10^{-1}$ over disk temperature range $3 - 7 \times 10^4$ K. Spiral arms facilitate inward mass flux by driving outward angular momentum transport. Gap-opening effects may further reduce the long-term accretion rate, albeit to confirm which requires global simulations evolved over much longer viscous timescales.

Figures

Figures reproduced from arXiv: 2505.13951 by the authors.

Figure 1
Figure 1. A snapshot of density, temperature and radial velocity distribution for the fiducial run T5e4 in quasi-steady state. The projected velocity streamlines are overlaid on the bottom panel. The left, middle and right columns correspond to the midplane, ϕ = π/2 (towards host) and ϕ = 0 (perpendicular to host) vertical distributions. All length units are in R⊙ [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Semi-transparent iso-density contours for the fiducial case showing the 3D structure of high density stellar envelope and density waves. The isodensity contours range from 10−11 to 10−7 g/cm3 in physical units. For visualization purpose, we are viewing the simulation domain from a bottom-up perspective. All length units are in R⊙. Significant density peaks can be seen along the spiral density waves. For a video show… view at source ↗
Figure 3
Figure 3. Left panel: time (over 100 snapshots within the final Ω−1 ) and azimuthally averaged 2D velocity streamlines and accretion rate ⟨M˙ ⟩(r, θ) profiles, for fiducial simulation T5e4. Color of streamline indicate the velocity magnitude. Right panel: ⟨M˙ ⟩(r, θ) averaged over different polar angle ranges, with red line being the total average. The red dashed and dotted lines indicate averages over the final 50 and 30 sna… view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: average radial profiles for different energy fluxes in the fiducial run T5e4. Definition of these variables and details of averaging see §2.2. to outflow. In summary, compared to the isotropic case, radiative feedback is enhanced at the pole and reduced in the midplane…
Figure 5
Figure 5. Figure 5: Left panel: time and azimuthally averaged 2D diffusive radiation flux streamlines and λdiff (r, θ) profiles, where λdiff (r, θ) indicates the fraction of radial gravity that radiation can effectively reduce, for fiducial simulation T5e4. Solid black lines are contours …
Figure 6
Figure 6. Figure 6: Similar to [PITH_FULL_IMAGE:figures/full_fig_p011_6.png]
Figure 8
Figure 8. Figure 8: Radial angular momentum fluxes defined in §2.2 for cases T3e4 and T7e4. Green dashed lines show the sum J˙ tot = J˙Rey +J˙ adv, which is expected to be a small constant along the accretion flow, although averages in the inner stel￾lar envelope within ∼ 40R⊙ may be subj…
Figure 9
Figure 9. Figure 9: Effective accretion parameter αeff for cases T3e4 and T7e4. Both cases yield αeff ∼ 0.1−1 within 50−200R⊙. αeff ≈ 1 [PITH_FULL_IMAGE:figures/full_fig_p012_9.png]
Figure 10
Figure 10. Figure 10: Midplane density distribution in a snapshot and in the data averaged over a dynamical timescale Ω−1 for run T3e4. Red dashed lines: fits of spiral wave front using ψ = 53◦ . Multiplication of this last expression by 2πr2 sin θ and integration over colatitude θ estimat…
Figure 11
Figure 11. Figure 11: Radial profile of midplane effective viscosity parameter calculated from Equation A5 for the run T3e4. Cantiello, M., Jermyn, A. S., & Lin, D. N. C. 2021, ApJ, 910, 94, doi: 10.3847/1538-4357/abdf4f Chen, Y.-X., Bailey, A., Stone, J., & Zhu, Z. 2022, ApJL, 939, L23, d…

Discussion (0). Sign in to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Using gravitational waves and multi-messenger Astronomy to reverse-engineer the properties of galactic nuclei

    astro-ph.HE 2025-06 conditional novelty 4.0 of 10

    The paper proposes that AGN-driven binary black hole merger rates, masses and spins can be used to infer the properties of AGN accretion disks and nuclear star clusters across cosmic time.

Reference graph

Works this paper leans on

76 extracted references · 11 canonical work pages · cited by 1 Pith paper

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    , "[+ 'd x .?^^ Xn qg ӒZJO,߾|&< <Tc] hcƏ6 kM >ژ l OG S#^I N ag ] *kn TIň <R s[nڵ

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    work page arXiv 2021

  4. [4]

    Ali-Dib , M., & Lin , D. N. C. 2023, , 10.1093/mnras/stad2774

    doi:10.1093/mnras/stad2774 2023

  5. [5]

    Artymowicz , P., Lin , D. N. C., & Wampler , E. J. 1993, , 409, 592, 10.1086/172690

    doi:10.1086/172690 1993

  6. [6]

    Begelman , M. C. 1978, , 184, 53, 10.1093/mnras/184.1.53

    doi:10.1093/mnras/184.1.53 1978

  7. [7]

    C., & Volonteri , M

    Begelman , M. C., & Volonteri , M. 2017, , 464, 1102, 10.1093/mnras/stw2446

    doi:10.1093/mnras/stw2446 2017

  8. [8]

    S., & Lin , D

    Cantiello , M., Jermyn , A. S., & Lin , D. N. C. 2021, , 910, 94, 10.3847/1538-4357/abdf4f

    doi:10.3847/1538-4357/abdf4f 2021

Show all 76 references
  1. [9]

    2022, , 939, L23, 10.3847/2041-8213/ac9b3e

    Chen , Y.-X., Bailey , A., Stone , J., & Zhu , Z. 2022, , 939, L23, 10.3847/2041-8213/ac9b3e

    2022 doi

  2. [10]

    Chen , Y.-X., Jiang , Y.-F., Goodman , J., & Lin , D. N. C. 2024, , 974, 106, 10.3847/1538-4357/ad6dd4

    2024 doi

  3. [11]

    Chen , Y.-X., Jiang , Y.-F., Goodman , J., & Ostriker , E. C. 2023, arXiv e-prints, arXiv:2302.10868, 10.48550/arXiv.2302.10868

    2023 doi arXiv

  4. [12]

    Chen , Y.-X., & Lin , D. N. C. 2024, , 967, 88, 10.3847/1538-4357/ad3c3a

    2024 doi

  5. [13]

    Chen , Y.-X., Zhang , X., Li , Y.-P., Li , H., & Lin , D. N. C. 2020, , 900, 44, 10.3847/1538-4357/abaab6

    2020 doi

  6. [14]

    2023, , 525, 2806, 10.1093/mnras/stad2269

    Choksi , N., Chiang , E., Fung , J., & Zhu , Z. 2023, , 525, 2806, 10.1093/mnras/stad2269

    2023 doi

  7. [15]

    J., & Cantiello , M

    Dittmann , A. J., & Cantiello , M. 2025, , 979, 245, 10.3847/1538-4357/ad9e92

    2025 doi

  8. [16]

    J., Cantiello , M., & Jermyn , A

    Dittmann , A. J., Cantiello , M., & Jermyn , A. S. 2021, , 916, 48, 10.3847/1538-4357/ac042c

    2021 doi

  9. [17]

    2024, arXiv e-prints, arXiv:2405.09380, 10.48550/arXiv.2405.09380

    Epstein-Martin , M., Tagawa , H., Haiman , Z., & Perna , R. 2024, arXiv e-prints, arXiv:2405.09380, 10.48550/arXiv.2405.09380

    2024 doi arXiv

  10. [18]

    Flammang , R. A. 1982, , 199, 833, 10.1093/mnras/199.4.833

    1982 doi

  11. [19]

    2024, arXiv e-prints, arXiv:2405.04456, 10.48550/arXiv.2405.04456

    Floris , A., Marziani , P., Panda , S., et al. 2024, arXiv e-prints, arXiv:2405.04456, 10.48550/arXiv.2405.04456

    2024 doi arXiv

  12. [20]

    L., Huang , J., Ali-Dib , M., et al

    Fryer , C. L., Huang , J., Ali-Dib , M., et al. 2025, , 537, 1556, 10.1093/mnras/staf130

    2025 doi

  13. [21]

    2019, , 887, 152, 10.3847/1538-4357/ab53da

    Fung , J., Zhu , Z., & Chiang , E. 2019, , 887, 152, 10.3847/1538-4357/ab53da

    2019 doi

  14. [23]

    F., & Stone, J

    Guo, M., Quataert, E., Squire, J., Hopkins, P. F., & Stone, J. M. 2025, Idealized Global Models of Accretion Disks with Strong Toroidal Magnetic Fields. 2505.12671

    2025 arXiv

  15. [24]

    1999, , 37, 487, 10.1146/annurev.astro.37.1.487

    Hamann , F., & Ferland , G. 1999, , 37, 487, 10.1146/annurev.astro.37.1.487

    1999 doi

  16. [25]

    T., Ferland , G

    Hamann , F., Korista , K. T., Ferland , G. J., Warner , C., & Baldwin , J. 2002, , 564, 592, 10.1086/324289

    2002 doi

  17. [26]

    Huang , J., Lin , D. N. C., & Shields , G. 2023, , 525, 5702, 10.1093/mnras/stad2642

    2023 doi

  18. [27]

    A., & Rogers , F

    Iglesias , C. A., & Rogers , F. J. 1996, , 464, 943, 10.1086/177381

    1996 doi

  19. [28]

    Inayoshi , K., Haiman , Z., & Ostriker , J. P. 2016, , 459, 3738, 10.1093/mnras/stw836

    2016 doi

  20. [29]

    2021, , 253, 49, 10.3847/1538-4365/abe303

    Jiang , Y.-F. 2021, , 253, 49, 10.3847/1538-4365/abe303

    2021 doi

  21. [30]

    2023, Galaxies, 11, 105, 10.3390/galaxies11050105

    ---. 2023, Galaxies, 11, 105, 10.3390/galaxies11050105

    2023 doi

  22. [31]

    2011, , 730, 45, 10.1088/0004-637X/730/1/45

    Jiang , Y.-F., & Goodman , J. 2011, , 730, 45, 10.1088/0004-637X/730/1/45

    2011 doi

  23. [32]

    M., & Davis , S

    Jiang , Y.-F., Stone , J. M., & Davis , S. W. 2014, , 213, 7, 10.1088/0067-0049/213/1/7

    2014 doi

  24. [33]

    M., & Zhu , Z

    Ju , W., Stone , J. M., & Zhu , Z. 2016, , 823, 81, 10.3847/0004-637X/823/2/81

    2016 doi

  25. [34]

    D., Tanaka , H., Muto , T., Tanigawa , T., & Takeuchi , T

    Kanagawa , K. D., Tanaka , H., Muto , T., Tanigawa , T., & Takeuchi , T. 2015, , 448, 994, 10.1093/mnras/stv025

    2015 doi

  26. [35]

    2014, , 788, 21, 10.1088/0004-637X/788/1/21

    Klahr , H., & Hubbard , A. 2014, , 788, 21, 10.1088/0004-637X/788/1/21

    2014 doi

  27. [36]

    Kormendy , J., & Ho , L. C. 2013, , 51, 511, 10.1146/annurev-astro-082708-101811

    2013 doi

  28. [37]

    M., & Youdin , A

    Krapp , L., Kratter , K. M., & Youdin , A. N. 2022, , 928, 156, 10.3847/1538-4357/ac5899

    2022 doi

  29. [38]

    M., Youdin , A

    Krapp , L., Kratter , K. M., Youdin , A. N., et al. 2024, , 973, 153, 10.3847/1538-4357/ad644a

    2024 doi

  30. [39]

    A., et al

    Lai , S., Bian , F., Onken , C. A., et al. 2022, , 513, 1801, 10.1093/mnras/stac1001

    2022 doi

  31. [40]

    Lesur , G., & Ogilvie , G. I. 2010, , 404, L64, 10.1111/j.1745-3933.2010.00836.x

    2010

  32. [41]

    2003, arXiv e-prints, astro, 10.48550/arXiv.astro-ph/0307084

    Levin , Y. 2003, arXiv e-prints, astro, 10.48550/arXiv.astro-ph/0307084

    2003 doi arXiv

  33. [42]

    Li , Y.-P., Chen , Y.-X., & Lin , D. N. C. 2023, , 526, 5346, 10.1093/mnras/stad3049

    2023 doi

  34. [43]

    M., Li , S., Li , H., & Li , J

    Li , Y.-P., Dempsey , A. M., Li , S., Li , H., & Li , J. 2021, , 911, 124, 10.3847/1538-4357/abed48

    2021 doi

  35. [44]

    Lin , D. N. C., & Papaloizou , J. 1980, , 191, 37, 10.1093/mnras/191.1.37

    1980 doi

  36. [45]

    1986, , 307, 395, 10.1086/164426

    ---. 1986, , 307, 395, 10.1086/164426

    1986 doi

  37. [46]

    1969, , 223, 690, 10.1038/223690a0

    Lynden-Bell , D. 1969, , 223, 690, 10.1038/223690a0

    1969 doi

  38. [47]

    2014, , 789, 77, 10.1088/0004-637X/789/1/77

    Lyra , W. 2014, , 789, 77, 10.1088/0004-637X/789/1/77

    2014 doi

  39. [48]

    MacLeod , M., & Lin , D. N. C. 2020, , 889, 94, 10.3847/1538-4357/ab64db

    2020 doi

  40. [49]

    Masset , F. S. 2001, , 558, 453, 10.1086/322446

    2001 doi

  41. [50]

    McKernan , B., Ford , K. E. S., Kocsis , B., Lyra , W., & Winter , L. M. 2014, , 441, 900, 10.1093/mnras/stu553

    2014 doi

  42. [51]

    McKernan , B., Ford , K. E. S., Lyra , W., & Perets , H. B. 2012, , 425, 460, 10.1111/j.1365-2966.2012.21486.x

    2012

  43. [52]

    2006, , 459, 85, 10.1051/0004-6361:20065216

    Nagao , T., Maiolino , R., & Marconi , A. 2006, , 459, 85, 10.1051/0004-6361:20065216

    2006 doi

  44. [53]

    P., Gressel , O., & Umurhan , O

    Nelson , R. P., Gressel , O., & Umurhan , O. M. 2013, , 435, 2610, 10.1093/mnras/stt1475

    2013 doi

  45. [54]

    1978, , 28, 91

    Paczynski , B. 1978, , 28, 91

    1978

  46. [55]

    Papaloizou , J., & Lin , D. N. C. 1984, , 285, 818, 10.1086/162561

    1984 doi

  47. [56]

    2011, , 192, 3, 10.1088/0067-0049/192/1/3

    Paxton , B., Bildsten , L., Dotter , A., et al. 2011, , 192, 3, 10.1088/0067-0049/192/1/3

    2011 doi

  48. [57]

    2013, , 208, 4, 10.1088/0067-0049/208/1/4

    Paxton , B., Cantiello , M., Arras , P., et al. 2013, , 208, 4, 10.1088/0067-0049/208/1/4

    2013 doi

  49. [58]

    B., et al

    Paxton , B., Schwab , J., Bauer , E. B., et al. 2018, , 234, 34, 10.3847/1538-4365/aaa5a8

    2018 doi

  50. [59]

    2019, , 243, 10, 10.3847/1538-4365/ab2241

    Paxton , B., Smolec , R., Schwab , J., et al. 2019, , 243, 10, 10.3847/1538-4365/ab2241

    2019 doi

  51. [60]

    2024, arXiv e-prints, arXiv:2410.14896, 10.48550/arXiv.2410.14896

    Sagynbayeva , S., Li , R., Kuznetsova , A., et al. 2024, arXiv e-prints, arXiv:2410.14896, 10.48550/arXiv.2410.14896

    2024 doi arXiv

  52. [61]

    J., et al

    Samsing , J., Bartos , I., D'Orazio , D. J., et al. 2022, , 603, 237, 10.1038/s41586-021-04333-1

    2022 doi

  53. [62]

    1986, , 219, 75, 10.1093/mnras/219.1.75

    Sawada , K., Matsuda , T., & Hachisu , I. 1986, , 219, 75, 10.1093/mnras/219.1.75

    1986 doi

  54. [63]

    C., Bildsten , L., & Jiang , Y.-F

    Schultz , W. C., Bildsten , L., & Jiang , Y.-F. 2022, , 924, L11, 10.3847/2041-8213/ac441f

    2022 doi

  55. [64]

    I., & Sunyaev , R

    Shakura , N. I., & Sunyaev , R. A. 1973, , 24, 337

    1973

  56. [65]

    2003, , 341, 501, 10.1046/j.1365-8711.2003.06431.x

    Sirko , E., & Goodman , J. 2003, , 341, 501, 10.1046/j.1365-8711.2003.06431.x

    2003

  57. [66]

    Spruit , H. C. 1987, , 184, 173

    1987

  58. [67]

    M., Tomida , K., White , C

    Stone , J. M., Tomida , K., White , C. J., & Felker , K. G. 2020, , 249, 4, 10.3847/1538-4365/ab929b

    2020 doi

  59. [68]

    2020, , 898, 25, 10.3847/1538-4357/ab9b8c

    Tagawa , H., Haiman , Z., & Kocsis , B. 2020, , 898, 25, 10.3847/1538-4357/ab9b8c

    2020 doi

  60. [69]

    A., Quataert , E., & Murray , N

    Thompson , T. A., Quataert , E., & Murray , N. 2005, , 630, 167, 10.1086/431923

    2005 doi

  61. [70]

    S., Flammang , R

    Thorne , K. S., Flammang , R. A., & Zytkow , A. N. 1981, , 194, 475, 10.1093/mnras/194.2.475

    1981 doi

  62. [71]

    C., Li , Y.-R., & Du , P

    Wang , J.-M., Liu , J.-R., Ho , L. C., Li , Y.-R., & Du , P. 2021, , 916, L17, 10.3847/2041-8213/ac0b46

    2021 doi

  63. [72]

    2023, , 954, 84, 10.3847/1538-4357/acdf48

    Wang , J.-M., Zhai , S., Li , Y.-R., et al. 2023, , 954, 84, 10.3847/1538-4357/acdf48

    2023 doi

  64. [73]

    2022, , 925, 121, 10.3847/1538-4357/ac3a69

    Wang , S., Jiang , L., Shen , Y., et al. 2022, , 925, 121, 10.3847/1538-4357/ac3a69

    2022 doi

  65. [74]

    Wang , Y., Lin , D. N. C., Zhang , B., & Zhu , Z. 2024, , 962, L7, 10.3847/2041-8213/ad20e5

    2024 doi

  66. [75]

    2018, , 480, 345, 10.1093/mnras/sty1763

    Xu , F., Bian , F., Shen , Y., et al. 2018, , 480, 345, 10.1093/mnras/sty1763

    2018 doi

  67. [76]

    2018, , 480, 4327, 10.1093/mnras/sty2151

    Xu , W., & Goodman , J. 2018, , 480, 4327, 10.1093/mnras/sty2151

    2018 doi

  68. [77]

    2021, , 508, 453, 10.1093/mnras/stab2517

    Zhu , Z., Jiang , Y.-F., Baehr , H., et al. 2021, , 508, 453, 10.1093/mnras/stab2517

    2021 doi

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.