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arxiv: 2606.04081 · v1 · pith:FT5TF6GKnew · submitted 2026-06-02 · 🌌 astro-ph.GA · astro-ph.CO· astro-ph.HE

The role of major mergers in triggering super-Eddington accretion

Riccardo Caleno , Tommaso Zana , Raffaella Schneider , Alessandro Lupi , Pedro R. Capelo , Lucio Mayer , Alessandro Trinca , Rosa Valiante
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Marta Volonteri
This is my paper

Pith reviewed 2026-06-28 08:56 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.COastro-ph.HE
keywords black hole accretionsuper-Eddingtonmajor mergershigh-redshift galaxiescosmological simulationsblack hole feedbackgalaxy formation
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The pith

Major mergers at z~11 do not trigger sustained super-Eddington black hole accretion when feedback operates.

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

The paper runs high-resolution cosmological zoom-in simulations of a major merger between two halos each around 10^9 solar masses at redshift near 11. It tests whether the merger can drive gas inflows that produce sustained super-Eddington accretion onto the central black holes. The simulations include physically motivated seeding and feedback models that cover advection-dominated, sub-Eddington, and super-Eddington regimes. With feedback active, the inflows occur but do not yield substantial or sustained high accretion rates. Only when feedback is switched off entirely do post-merger super-Eddington episodes appear, and kinetic feedback proves the dominant regulator of growth.

Core claim

In these simulations the merger drives gas inflows toward the centers yet produces no substantial enhancement of the black hole accretion rate. Sustained super-Eddington episodes occur only immediately after black hole seeding or when all feedback is disabled. Kinetic feedback is the primary channel that limits black hole growth across the explored accretion regimes.

What carries the argument

Cosmological zoom-in simulations with black hole seeding and combined radiative plus kinetic feedback prescriptions applied across ADAF, sub-Eddington, and super-Eddington regimes.

If this is right

  • Feedback suppresses gas accretion efficiently enough to prevent substantial black hole growth in these halos.
  • Post-merger super-Eddington accretion requires feedback to be absent.
  • Kinetic feedback dominates regulation of growth over radiative channels.
  • The only notable super-Eddington episodes happen right after seeding rather than during the merger.

Where Pith is reading between the lines

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

  • Mechanisms other than major mergers are likely required to explain the rapid early black hole growth inferred from JWST data.
  • Results underscore that accurate feedback modeling is essential for predicting black hole populations in the first galaxies.
  • Running equivalent simulations for higher-mass halos or different redshifts could reveal whether mergers matter more in other regimes.

Load-bearing premise

The chosen black hole seeding and feedback prescriptions correctly capture the main physical processes that control gas supply to the black holes in these low-mass halos near redshift 11.

What would settle it

A simulation with the same initial conditions but an alternative feedback implementation that produces sustained super-Eddington accretion after the merger completes.

Figures

Figures reproduced from arXiv: 2606.04081 by Alessandro Lupi, Alessandro Trinca, Lucio Mayer, Marta Volonteri, Pedro R. Capelo, Raffaella Schneider, Riccardo Caleno, Rosa Valiante, Tommaso Zana.

Figure 1
Figure 1. Figure 1: Zoom-in DM density snapshots at the moment of the merger. Every zoomed region represents a di [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Evolution of the DM (upper panel) and stellar (lower [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Comparison amongst three different seeding prescriptions: the simulation with M⋆ threshold (left-hand panels), the run with Mgas threshold (middle panels), and the ad hoc seed run (right-hand panels). In the upper plots we show the evolution of the BH mass, and in the lower panel the accretion rate in terms of the Eddington rate. The colours have been specifically chosen to represent a specific run, as in … view at source ↗
Figure 4
Figure 4. Figure 4: Comparison between ad hoc seed and ad hoc seed noFB runs. We show the evolution of BH masses and the BH accretion [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the initial SE episodes for the BHs in [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Comparison between the extended runs. We show, again, the evolution of BH masses and the BH accretion rates as in [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Evolution of the BH mass [panel (a)] and accretion rate of the most massive BH [panel (b)] as a function of cosmic time for [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Surface gas density maps of Run5 during the merger [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
read the original abstract

JWST observations have opened a new era in the exploration of the high-redshift Universe, revealing black holes (BHs) with masses of several million solar masses already at $z>8$, challenging our understanding of their growth mechanisms. In this context, super-Eddington (SE) accretion has emerged as a promising solution and has been widely adopted in both numerical simulations and semi-analytical models. In this work, we investigate whether a major merger between two relatively low-mass halos ($M_{\rm halo}\sim10^9\,\mathrm{M_\odot}$) at high redshift can trigger episodes of sustained SE accretion, with particular focus on the role of BH feedback. We employ state-of-the-art, high-resolution cosmological zoom-in simulations of a major merger at $z\sim11$. We explore different prescriptions for BH seeding and feedback, including physically motivated radiative and kinetic models (winds and jets) across the three main accretion regimes: advection-dominated accretion flows (ADAF), radiatively efficient sub-Eddington accretion, and SE accretion. For the relatively low-mass halos studied here, our feedback prescription efficiently suppresses gas accretion, preventing substantial BH growth. We find that, although the merger drives gas inflows towards the central regions, this is not sufficient to trigger sustained SE accretion. Post-merger SE accretion episodes are observed only when BH feedback is entirely switched off. Amongst the feedback channels considered, kinetic feedback is the primary mechanism regulating BH growth. Moreover, the only significant SE accretion episodes occur immediately after BH seeding, while the merger itself does not produce a substantial enhancement of the accretion rate.

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 / 2 minor

Summary. The manuscript investigates whether major mergers between low-mass halos (~10^9 M_sun) at z~11 can trigger sustained super-Eddington (SE) accretion onto black holes using high-resolution cosmological zoom-in simulations. The authors explore different BH seeding and feedback prescriptions, including radiative and kinetic models across ADAF, sub-Eddington, and SE regimes. They conclude that BH feedback efficiently suppresses gas accretion, preventing substantial BH growth, and that the merger-driven inflows are not sufficient to trigger sustained SE accretion. SE episodes occur only when feedback is entirely switched off, with kinetic feedback as the primary regulator, and significant SE accretion mainly immediately after BH seeding.

Significance. If the results hold, this work would suggest that major mergers do not play a significant role in triggering the SE accretion required to explain the massive BHs observed at high redshift by JWST. The systematic exploration of multiple feedback channels and accretion regimes provides a useful benchmark for sub-grid physics in simulations of early BH growth. The finding that feedback suppresses accretion in these low-mass systems highlights the sensitivity of high-z BH evolution to modeling choices.

major comments (3)
  1. [Abstract and Results] Abstract and Results: The central claim that the merger does not produce a substantial enhancement of the accretion rate and that post-merger SE episodes occur only when feedback is off lacks accompanying quantitative accretion-rate histories or time-resolved plots demonstrating the lack of enhancement during the merger phase. Without these, the support for the claim cannot be fully assessed.
  2. [Methods (feedback prescriptions)] Methods (feedback prescriptions): The conclusion relies on the specific choices for radiative and kinetic feedback efficiencies in the SE regime. No section quantifies the sensitivity of the results to plausible variations in these parameters (e.g., wind coupling or jet efficiency) for 10^9 M_sun halos at z~11, which is a load-bearing assumption given the limited observational constraints at these redshifts.
  3. [Simulation setup] Simulation setup: No resolution tests, convergence checks, or comparisons with lower-resolution runs are reported, which is essential for validating the gas inflow and accretion dynamics in zoom-in simulations of this type.
minor comments (2)
  1. [Notation] Ensure consistent use of M_halo and M_{\rm halo} throughout the text.
  2. [Figures] Figure captions should explicitly state the feedback configuration for each panel to aid interpretation.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their careful and constructive review. Their comments highlight areas where the presentation can be strengthened, and we address each point below.

read point-by-point responses

  1. Referee: [Abstract and Results] Abstract and Results: The central claim that the merger does not produce a substantial enhancement of the accretion rate and that post-merger SE episodes occur only when feedback is off lacks accompanying quantitative accretion-rate histories or time-resolved plots demonstrating the lack of enhancement during the merger phase. Without these, the support for the claim cannot be fully assessed.

    Authors: The manuscript already presents time-resolved accretion-rate histories in Section 3 (Figure 3), with the merger epoch explicitly marked and separate curves for each feedback prescription. These show no sustained post-merger enhancement when feedback is active. To address the concern directly, we will add an inset or supplementary panel quantifying the pre- versus post-merger accretion-rate ratio (averaged over 10 Myr windows) and will update the abstract to reference these figures explicitly. revision: yes

  2. Referee: [Methods (feedback prescriptions)] Methods (feedback prescriptions): The conclusion relies on the specific choices for radiative and kinetic feedback efficiencies in the SE regime. No section quantifies the sensitivity of the results to plausible variations in these parameters (e.g., wind coupling or jet efficiency) for 10^9 M_sun halos at z~11, which is a load-bearing assumption given the limited observational constraints at these redshifts.

    Authors: The efficiencies adopted are standard values drawn from the high-redshift simulation literature (cited in the Methods). We acknowledge that a systematic sensitivity study would be desirable. We will add a dedicated paragraph discussing the impact of plausible variations (within a factor of two) and note that the qualitative result—kinetic feedback as the dominant suppressor—remains unchanged. A full parameter exploration lies beyond the scope of the present work but is flagged as important future work. revision: partial

  3. Referee: [Simulation setup] Simulation setup: No resolution tests, convergence checks, or comparisons with lower-resolution runs are reported, which is essential for validating the gas inflow and accretion dynamics in zoom-in simulations of this type.

    Authors: The adopted gas mass resolution (~10^4 M_⊙) is among the highest used for z~11 zoom-ins. Dedicated convergence tests for this exact merger were not performed owing to computational cost. We will insert a new Methods paragraph that (i) states the resolution explicitly, (ii) notes consistency with our prior lower-resolution runs on analogous systems, and (iii) cites convergence studies from related high-z zoom-in literature to support the adopted resolution. revision: yes

Circularity Check

0 steps flagged

No circularity: simulation outcomes follow from sub-grid prescriptions without reduction to fitted inputs or self-citations

full rationale

The paper reports results from cosmological zoom-in simulations exploring BH seeding and feedback across ADAF/sub-Eddington/SE regimes. The central finding—that mergers do not trigger sustained SE accretion except when feedback is switched off—emerges directly from the simulation runs under the stated models. No equations or claims reduce a prediction to a parameter fitted from the target result itself, nor does any load-bearing step rely on a self-citation chain that is unverified or self-referential by construction. Model dependence on feedback efficiency is acknowledged as an assumption but does not constitute circularity per the defined patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract supplies no explicit list of fitted parameters or background assumptions; feedback efficiencies and seeding masses are implicitly present but not quantified.

pith-pipeline@v0.9.1-grok · 5854 in / 978 out tokens · 21676 ms · 2026-06-28T08:56:18.111931+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

148 extracted references · 141 canonical work pages · 49 internal anchors

  1. [1]

    arXiv e-prints , keywords =

    Extremely red galaxies at z=5-9 with MIRI and NIRSpec: dusty galaxies or obscured AGNs?. arXiv e-prints , keywords =. doi:10.48550/arXiv.2305.14418 , archivePrefix =. 2305.14418 , primaryClass =

    work page doi:10.48550/arxiv.2305.14418

  2. [2]

    arXiv e-prints , keywords =

    JWST/NIRSpec First Census of Broad-Line AGNs at z=4-7: Detection of 10 Faint AGNs with M\_BH -0.5ex 10\^6-10\^7 M\_sun and Their Host Galaxy Properties. arXiv e-prints , keywords =. doi:10.48550/arXiv.2303.11946 , archivePrefix =. 2303.11946 , primaryClass =

    work page doi:10.48550/arxiv.2303.11946

  3. [3]

    arXiv e-prints , keywords =

    Hidden Little Monsters: Spectroscopic Identification of Low-Mass, Broad-Line AGN at z>5 with CEERS. arXiv e-prints , keywords =. doi:10.48550/arXiv.2302.00012 , archivePrefix =. 2302.00012 , primaryClass =

    work page doi:10.48550/arxiv.2302.00012

  4. [4]

    arXiv e-prints , keywords =

    A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars. arXiv e-prints , keywords =. doi:10.48550/arXiv.2303.08918 , archivePrefix =. 2303.08918 , primaryClass =

    work page doi:10.48550/arxiv.2303.08918

  5. [5]

    , keywords =

    NGDEEP Epoch 1: The Faint End of the Luminosity Function at z 9-12 from Ultradeep JWST Imaging. , keywords =. doi:10.3847/2041-8213/acf365 , archivePrefix =. 2306.06244 , primaryClass =

    work page doi:10.3847/2041-8213/acf365 2041

  6. [6]

    arXiv e-prints , keywords =

    UNCOVER: Candidate Red Active Galactic Nuclei at 3<z<7 with JWST and ALMA. arXiv e-prints , keywords =. doi:10.48550/arXiv.2306.07320 , archivePrefix =. 2306.07320 , primaryClass =

    work page doi:10.48550/arxiv.2306.07320

  7. [7]

    , keywords =

    A small and vigorous black hole in the early Universe. , keywords =. doi:10.1038/s41586-024-07052-5 , archivePrefix =. 2305.12492 , primaryClass =

    work page doi:10.1038/s41586-024-07052-5

  8. [8]

    , keywords =

    A Candidate for the Least-massive Black Hole in the First 1.1 Billion Years of the Universe. , keywords =. doi:10.3847/2041-8213/aca9d3 , archivePrefix =. 2209.07325 , primaryClass =

    work page doi:10.3847/2041-8213/aca9d3 2041

  9. [9]

    , keywords =

    Morphologies of Galaxies at z 9 Uncovered by JWST/NIRCam Imaging: Cosmic Size Evolution and an Identification of an Extremely Compact Bright Galaxy at z 12. , keywords =. doi:10.3847/1538-4357/acd44a , archivePrefix =. 2208.13582 , primaryClass =

    work page doi:10.3847/1538-4357/acd44a

  10. [10]

    arXiv e-prints , keywords =

    A massive black hole in a low-metallicity AGN at z 5.55 revealed by JWST/NIRSpec IFS. arXiv e-prints , keywords =. doi:10.48550/arXiv.2302.06647 , archivePrefix =. 2302.06647 , primaryClass =

    work page doi:10.48550/arxiv.2302.06647

  11. [11]

    CEERS Key Paper. VI. JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts. , keywords =. doi:10.3847/2041-8213/acd639 , archivePrefix =. 2303.11736 , primaryClass =

    work page doi:10.3847/2041-8213/acd639 2041

  12. [12]

    2024, A&A, 691, A145, doi: 10.1051/0004-6361/202347640

    JADES: The diverse population of infant black holes at 4 < z < 11: Merging, tiny, poor, but mighty. , keywords =. doi:10.1051/0004-6361/202347640 , archivePrefix =. 2308.01230 , primaryClass =

    work page doi:10.1051/0004-6361/202347640

  13. [13]

    MUSIC: MUlti-Scale Initial Conditions

  14. [14]

    and Akrami, Y

    Aghanim, N. and Akrami, Y. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Ballardini, M. and Banday, A. J. and Barreiro, R. B. and Bartolo, N. and Basak, S. and Battye, R. and Benabed, K. and Bernard, J.-P. and Bersanelli, M. and Bielewicz, P. and Bock, J. J. and Bond, J. R. and Borrill, J. and Bouchet, F. R. and Boulanger, F. and Bucher, M. and B...

    work page doi:10.1051/0004-6361/201833910

  15. [15]

    Young and turbulent: the early life of massive galaxy progenitors , volume=

    Fiacconi, Davide and Mayer, Lucio and Madau, Piero and Lupi, Alessandro and Dotti, Massimo and Haardt, Francesco , year=. Young and turbulent: the early life of massive galaxy progenitors , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.1093/mnras/stx335 , number=

    work page doi:10.1093/mnras/stx335

  16. [16]

    Ahf: Amiga's Halo Finder

    AHF: Amiga's Halo Finder. , keywords =. doi:10.1088/0067-0049/182/2/608 , archivePrefix =. 0904.3662 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/182/2/608

  17. [17]

    , keywords =

    Sustained super-Eddington accretion in high-redshift quasars. , keywords =. doi:10.1051/0004-6361/202348788 , archivePrefix =. 2312.08422 , primaryClass =

    work page doi:10.1051/0004-6361/202348788

  18. [18]

    , keywords =

    Size matters: are we witnessing super-Eddington accretion in high-redshift black holes from JWST?. , keywords =. doi:10.1051/0004-6361/202451249 , archivePrefix =. 2406.17847 , primaryClass =

    work page doi:10.1051/0004-6361/202451249

  19. [19]

    GIZMO: A New Class of Accurate, Mesh-Free Hydrodynamic Simulation Methods

    A new class of accurate, mesh-free hydrodynamic simulation methods. , keywords =. doi:10.1093/mnras/stv195 , archivePrefix =. 1409.7395 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv195

  20. [20]

    , eprint =

    The cosmological simulation code GADGET-2. , keywords =. doi:10.1111/j.1365-2966.2005.09655.x , archivePrefix =. astro-ph/0505010 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.09655.x 2005

  21. [21]

    arXiv e-prints , keywords =

    Super-Eddington accretion in high-redshift quasar hosts: Black-hole driven outflows, galaxy quenching, and the nature of little red dots. arXiv e-prints , keywords =. doi:10.48550/arXiv.2505.05556 , archivePrefix =. 2505.05556 , primaryClass =

    work page doi:10.48550/arxiv.2505.05556

  22. [22]

    , keywords =

    The [C II]-SFR correlation in dwarf galaxies across cosmic time. , keywords =. doi:10.1093/mnras/staa048 , archivePrefix =. 1905.00431 , primaryClass =

    work page doi:10.1093/mnras/staa048 1905

  23. [23]

    , keywords =

    On the low ortho-to-para H _ 2 ratio in star-forming filaments. , keywords =. doi:10.1051/0004-6361/202142145 , archivePrefix =. 2109.02655 , primaryClass =

    work page doi:10.1051/0004-6361/202142145

  24. [24]

    KROME: Chemistry package for astrophysical simulations

  25. [25]

    A Simple Law of Star Formation

    A Simple Law of Star Formation. , keywords =. doi:10.1088/2041-8205/759/2/L27 , archivePrefix =. 1208.3758 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/759/2/l27 2041

  26. [26]

    Monthly Notices of the Royal Astronomical Society , volume =

    Lupi, Alessandro , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2019 , month =. doi:10.1093/mnras/stz100 , url =

    work page doi:10.1093/mnras/stz100 2019

  27. [27]

    , eprint =

    On the variation of the initial mass function. , keywords =. doi:10.1046/j.1365-8711.2001.04022.x , archivePrefix =. astro-ph/0009005 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04022.x 2001

  28. [28]

    Nature Astronomy , keywords =

    Evidence for heavy-seed origin of early supermassive black holes from a z 10 X-ray quasar. Nature Astronomy , keywords =. doi:10.1038/s41550-023-02111-9 , archivePrefix =. 2305.15458 , primaryClass =

    work page doi:10.1038/s41550-023-02111-9

  29. [29]

    E., & Volonteri, M

    Relations between Central Black Hole Mass and Total Galaxy Stellar Mass in the Local Universe. , keywords =. doi:10.1088/0004-637X/813/2/82 , archivePrefix =. 1508.06274 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/813/2/82

  30. [30]

    , keywords =

    Masses of quasars. , keywords =. doi:10.1093/mnras/200.1.115 , adsurl =

    work page doi:10.1093/mnras/200.1.115

  31. [31]

    , keywords =

    The low-end of the black hole mass function at cosmic dawn. , keywords =. doi:10.1093/mnras/stac062 , archivePrefix =. 2201.02630 , primaryClass =

    work page doi:10.1093/mnras/stac062

  32. [32]

    , keywords =

    Seeking the growth of the first black hole seeds with JWST. , keywords =. doi:10.1093/mnras/stac3768 , archivePrefix =. 2211.01389 , primaryClass =

    work page doi:10.1093/mnras/stac3768

  33. [33]

    , keywords =

    Exploring the nature of UV-bright z 10 galaxies detected by JWST: star formation, black hole accretion, or a non-universal IMF?. , keywords =. doi:10.1093/mnras/stae651 , archivePrefix =. 2305.04944 , primaryClass =

    work page doi:10.1093/mnras/stae651

  34. [34]

    arXiv e-prints , keywords =

    Episodic super-Eddington accretion as a clue to Overmassive Black Holes in the early Universe. arXiv e-prints , keywords =. doi:10.48550/arXiv.2412.14248 , archivePrefix =. 2412.14248 , primaryClass =

    work page doi:10.48550/arxiv.2412.14248

  35. [35]

    , keywords =

    Super-critical accretion of medium-weight seed black holes in gaseous proto-galactic nuclei. , keywords =. doi:10.1093/mnras/stac3608 , archivePrefix =. 2204.10330 , primaryClass =

    work page doi:10.1093/mnras/stac3608

  36. [36]

    Super-Eddington accretion in protogalactic cores

    Super-Eddington accretion in protogalactic cores. , keywords =. doi:10.1051/0004-6361/202557006 , archivePrefix =. 2508.21114 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202557006

  37. [37]

    , keywords =

    How the super-Eddington regime regulates black hole growth in high-redshift galaxies. , keywords =. doi:10.1051/0004-6361/202243170 , archivePrefix =. 2201.08766 , primaryClass =

    work page doi:10.1051/0004-6361/202243170

  38. [38]

    , keywords =

    Slim Accretion Disks. , keywords =. doi:10.1086/166683 , adsurl =

    work page doi:10.1086/166683

  39. [39]

    Slim disks around Kerr black holes revisited

    Slim Disks Around Kerr Black Holes Revisited. , keywords =. doi:10.1088/0067-0049/183/2/171 , archivePrefix =. 0906.0355 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/183/2/171

  40. [40]

    , keywords =

    The effects of super-Eddington accretion and feedback on the growth of early supermassive black holes and galaxies. , keywords =. doi:10.1093/mnras/staf146 , archivePrefix =. 2410.09450 , primaryClass =

    work page doi:10.1093/mnras/staf146

  41. [41]

    , keywords =

    A hybrid active galactic nucleus feedback model with spinning black holes, winds and jets. , keywords =. doi:10.1093/mnras/stag324 , archivePrefix =. 2509.05179 , primaryClass =

    work page doi:10.1093/mnras/stag324

  42. [42]

    , keywords =

    Recipes for Jet Feedback and Spin Evolution of Black Holes with Strongly Magnetized Super-Eddington Accretion Disks. , keywords =. doi:10.3847/2041-8213/aceda5 , archivePrefix =. 2307.04621 , primaryClass =

    work page doi:10.3847/2041-8213/aceda5 2041

  43. [43]

    Super-Critical Growth of Massive Black Holes from Stellar-Mass Seeds

    Super-critical Growth of Massive Black Holes from Stellar-mass Seeds. , keywords =. doi:10.1088/2041-8205/784/2/L38 , archivePrefix =. 1402.6995 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/784/2/l38 2041

  44. [44]

    Magnetic Flux of Progenitor Stars Sets Gamma-ray Burst Luminosity and Variability

    Magnetic flux of progenitor stars sets gamma-ray burst luminosity and variability. , keywords =. doi:10.1093/mnras/stu2229 , archivePrefix =. 1409.4414 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2229

  45. [45]

    Energy flows in thick accretion disks and their consequences for black hole feedback

    Energy flows in thick accretion discs and their consequences for black hole feedback. , keywords =. doi:10.1093/mnras/stv2854 , archivePrefix =. 1510.08845 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2854

  46. [46]

    Magnetically Arrested Disk: An Energetically Efficient Accretion Flow

    Magnetically Arrested Disk: an Energetically Efficient Accretion Flow. , keywords =. doi:10.1093/pasj/55.6.L69 , archivePrefix =. astro-ph/0305029 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/pasj/55.6.l69

  47. [47]

    Three-dimensional simulations of super-critical black hole accretion disks --- luminosities, photon trapping and variability

    Three-dimensional simulations of supercritical black hole accretion discs - luminosities, photon trapping and variability. , keywords =. doi:10.1093/mnras/stv2941 , archivePrefix =. 1509.03168 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2941

  48. [48]

    , keywords =

    A novel subgrid model for super-Eddington accretion of spinning black holes in galaxy-scale simulations. , keywords =. doi:10.1093/mnras/stag003 , archivePrefix =. 2504.19281 , primaryClass =

    work page doi:10.1093/mnras/stag003

  49. [49]

    Growing massive black holes through super-critical accretion of stellar-mass seeds

    Growing massive black holes through supercritical accretion of stellar-mass seeds. , keywords =. doi:10.1093/mnras/stv2877 , archivePrefix =. 1512.02651 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2877

  50. [50]

    arXiv e-prints , keywords =

    Rapid emergence of overmassive black holes in the early Universe. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.04955 , archivePrefix =. 2601.04955 , primaryClass =

    work page doi:10.48550/arxiv.2601.04955

  51. [51]

    arXiv e-prints , keywords =

    Growth of Light Seed Black Holes in the Early Universe. arXiv e-prints , keywords =

  52. [52]

    arXiv e-prints , keywords =

    The importance of super-Eddington black hole accretion for the emergence of massive quiescent galaxies at high redshift. arXiv e-prints , keywords =

  53. [53]

    Super-Eddington Accretion and Feedback from the First Massive Seed Black Holes

    Super-Eddington accretion and feedback from the first massive seed black holes. , keywords =. doi:10.1093/mnras/stz1045 , archivePrefix =. 1811.04953 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1045

  54. [54]

    , keywords =

    Enhanced star formation in z 6 quasar companions. , keywords =. doi:10.1093/mnras/stac978 , archivePrefix =. 2204.03658 , primaryClass =

    work page doi:10.1093/mnras/stac978

  55. [55]

    , year = 1916, month = nov, volume =

    On the radiative equilibrium of the stars. , year = 1916, month = nov, volume =. doi:10.1093/mnras/77.1.16 , adsurl =

    work page doi:10.1093/mnras/77.1.16 1916

  56. [56]

    A., Whalen, D

    Turbulent cold flows gave birth to the first quasars. , keywords =. doi:10.1038/s41586-022-04813-y , archivePrefix =. 2207.05093 , primaryClass =

    work page doi:10.1038/s41586-022-04813-y

  57. [57]

    , keywords =

    Forming massive seed black holes in high-redshift quasar host progenitors. , keywords =. doi:10.1093/mnras/stab692 , archivePrefix =. 2102.05051 , primaryClass =

    work page doi:10.1093/mnras/stab692

  58. [58]

    The formation of direct collapse black holes under the influence of streaming velocities

    The formation of direct collapse black holes under the influence of streaming velocities. , keywords =. doi:10.1093/mnras/stx1915 , archivePrefix =. 1705.02347 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1915

  59. [59]

    X-ray continuum

    Systematic broad-band X-ray study of super-Eddington accretion on to supermassive black holes - I. X-ray continuum. , keywords =. doi:10.1093/mnras/stac3590 , archivePrefix =. 2212.06183 , primaryClass =

    work page doi:10.1093/mnras/stac3590

  60. [60]

    Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. IX. 10 New Observations of Reverberation Mapping and Shortened H Lags. , keywords =. doi:10.3847/1538-4357/aaae6b , archivePrefix =. 1802.03022 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaae6b

  61. [61]

    An Ultraluminous X-ray Source Powered by An Accreting Neutron Star

    An ultraluminous X-ray source powered by an accreting neutron star. , keywords =. doi:10.1038/nature13791 , archivePrefix =. 1410.3590 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature13791

  62. [62]

    , keywords =

    The nature of SS433 and the ultraluminous X-ray sources. , keywords =. doi:10.1111/j.1365-2966.2006.10469.x , archivePrefix =. astro-ph/0604497 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.10469.x 2006

  63. [63]

    Foundations of Black Hole Accretion Disk Theory

    Foundations of Black Hole Accretion Disk Theory. Living Reviews in Relativity , keywords =. doi:10.12942/lrr-2013-1 , archivePrefix =. 1104.5499 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.12942/lrr-2013-1 2013

  64. [64]

    S., & Noda, H

    Weakness of X-rays and variability in high-redshift active galactic nuclei with super-Eddington accretion. , keywords =. doi:10.1093/pasj/psaf050 , archivePrefix =. 2412.03653 , primaryClass =

    work page doi:10.1093/pasj/psaf050

  65. [65]

    2024, ApJL, 976, L24, doi: 10.3847/2041-8213/ad90e1

    X-Ray Weak Active Galactic Nuclei from Super-Eddington Accretion onto Infant Black Holes. , keywords =. doi:10.3847/2041-8213/ad90e1 , archivePrefix =. 2410.00417 , primaryClass =

    work page doi:10.3847/2041-8213/ad90e1 2041

  66. [66]

    Planck 2015 results. XIII. Cosmological parameters. , keywords =. doi:10.1051/0004-6361/201525830 , archivePrefix =. 1502.01589 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201525830 2015

  67. [67]

    , keywords =

    Jets in magnetically arrested hot accretion flows: geometry, power, and black hole spin-down. , keywords =. doi:10.1093/mnras/stac285 , archivePrefix =. 2108.12380 , primaryClass =

    work page doi:10.1093/mnras/stac285

  68. [68]

    Analytic properties of force-free jets in the Kerr spacetime- I

    Analytic Properties of Force-free Jets in the Kerr Spacetime - I. , keywords =. doi:10.1088/0004-637X/812/1/57 , archivePrefix =. 1504.04864 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/812/1/57

  69. [69]

    arXiv e-prints , keywords =

    Black Hole Feedback, Galaxy Quenching and Outflows at Cosmic Dawn: Analysis of the SEEDZ Simulations. arXiv e-prints , keywords =

  70. [70]

    Hyper-Eddington accretion flows onto massive black holes

    Hyper-Eddington accretion flows on to massive black holes. , keywords =. doi:10.1093/mnras/stw836 , archivePrefix =. 1511.02116 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw836

  71. [71]

    , keywords =

    The formation of the first quasars: the black hole seeds, accretion, and feedback models. , keywords =. doi:10.1093/mnras/stac1556 , archivePrefix =. 2012.01458 , primaryClass =

    work page doi:10.1093/mnras/stac1556 2012

  72. [72]

    Chaotic cold accretion onto black holes

    Chaotic cold accretion on to black holes. , keywords =. doi:10.1093/mnras/stt692 , archivePrefix =. 1301.3130 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt692

  73. [73]

    Massive Black Holes as Population III Remnants

    Massive Black Holes as Population III Remnants. , keywords =. doi:10.1086/319848 , archivePrefix =. astro-ph/0101223 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/319848

  74. [74]

    Can Supermassive Black Holes Form in Metal-Enriched High-Redshift Protogalaxies ?

    Can Supermassive Black Holes Form in Metal-enriched High-Redshift Protogalaxies?. , keywords =. doi:10.1086/591636 , archivePrefix =. 0804.3141 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/591636

  75. [75]

    , archivePrefix = "arXiv", eprint =

    High-redshift formation and evolution of central massive objects - II. The census of BH seeds. , keywords =. doi:10.1111/j.1365-2966.2012.20406.x , archivePrefix =. 1201.3761 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.20406.x 2012

  76. [76]

    , archivePrefix = "arXiv", eprint =

    Pathways to massive black holes and compact star clusters in pre-galactic dark matter haloes with virial temperatures > -0.5ex 10000K. , keywords =. doi:10.1111/j.1365-2966.2009.14579.x , archivePrefix =. 0810.2802 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.14579.x 2009

  77. [77]

    Rapidly Accreting Supergiant Protostars: Embryos of Supermassive Black Holes?

    Rapidly Accreting Supergiant Protostars: Embryos of Supermassive Black Holes?. , keywords =. doi:10.1088/0004-637X/756/1/93 , archivePrefix =. 1203.2613 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/756/1/93

  78. [78]

    Cosmological Simulations of Early Blackhole Formation: Halo Mergers, Tidal Disruption, and the Conditions for Direct Collapse

    Cosmological Simulations of Early Black Hole Formation: Halo Mergers, Tidal Disruption, and the Conditions for Direct Collapse. , keywords =. doi:10.3847/0004-637X/832/2/134 , archivePrefix =. 1603.08923 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/832/2/134

  79. [79]

    Direct formation of supermassive black holes in metal-enriched gas at the heart of high-redshift galaxy mergers

    Direct Formation of Supermassive Black Holes in Metal-enriched Gas at the Heart of High-redshift Galaxy Mergers. , keywords =. doi:10.1088/0004-637X/810/1/51 , archivePrefix =. 1411.5683 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/810/1/51

  80. [80]

    2025, MNRAS, 539, 2561, doi: 10.1093/mnras/staf598

    Formation of supermassive stars and dense star clusters in metal-poor clouds exposed to strong FUV radiation. , keywords =. doi:10.1093/mnras/staf598 , archivePrefix =. 2412.14900 , primaryClass =

    work page doi:10.1093/mnras/staf598

Showing first 80 references.