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Observational properties of regular black holes in Asymptotic Safety

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Pith's one-line read As the asymptotic-safety parameter ξ grows, the shadow shrinks, the innermost orbit moves inward, and the accretion disk becomes brighter and more efficient than in Schwarzschild.

arxiv 2504.12072 v2 pith:H32QQ2DZ submitted 2025-04-16 gr-qc

Abdybek Urmanov , Hrishikesh Chakrabarty , Daniele Malafarina This is my paper · ORCID
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keywords schwarzschildaccretionmetricpropertiesasymptoticblackdiskdisks
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The pith

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

The reading

The paper studies a specific model of a black hole that comes from asymptotic safety, a theory that tries to describe gravity at very small distances. The metric, taken from earlier work, looks exactly like Schwarzschild far away, but has a free parameter ξ that controls how strongly quantum effects modify spacetime near the center. The authors compute how light and matter move in this spacetime and then use standard disk physics to predict what a glowing gas disk around such an object would look like.

They find a consistent trend: as ξ grows, the photon ring and the shadow shrink, the innermost stable orbit moves inward, and the disk can extend closer to the center. The disk therefore produces more flux, higher luminosity, a higher accretion efficiency, and a spectrum shifted to higher frequencies. Their iron line simulations show a slightly weaker blue peak and a slightly longer red tail than Schwarzschild.

The authors are careful about some limitations: the spacetime is not actually regular at r=0 (the Kretschmann scalar diverges), the model is non-rotating, and for a range of ξ there are two marginally stable orbits, so the inner part of the disk is not included in their flux calculation. They also note that if the quantum cutoff is at the Planck scale, ξ would be very small and all these deviations would be tiny.

Extended reading notes

Core claim

For the asymptotic-safety black hole metric (Eq. 2), the photon ring and shadow radii shrink, the ISCO moves inward, and the accretion disk's radiative flux, spectral luminosity, and efficiency all increase with the free parameter ξ, while the Kα iron line develops a lower blue peak and longer red tail relative to Schwarzschild (Abstract, Secs. III-V).

Load-bearing premise

The paper's flux, luminosity, and efficiency results assume the thin accretion disk emits only from r ≥ r_isco and that the stress vanishes at the inner edge; for ξ/M0^2 in (0.67, 1.05), where the paper itself finds a second stable circular orbit at smaller radii, that inner region is explicitly excluded (Sec. IV, after Fig. 8). If particles can circularize again there, the predicted brightening and efficiency gain could be significantly altered.

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Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

The analysis depends on the cited asymptotically safe metric and the standard thin-disk model; the only tuned quantity is ξ, and the only ad hoc modeling choice is the neglect of the inner stable disk region in the two-ISCO parameter range.

free parameters (2)
  • ξ (asymptotic safety UV cutoff parameter) = Varied in figures, e.g., 0.3, 2/3 (in units of M0^2); expected to be extremely small if the cutoff is at the Planck…
    Single free parameter controlling all deviations from Schwarzschild; all claims are monotonic in ξ.
  • α (disk emissivity index) = 3 and 4
    Used in iron line profiles to model the radial emissivity; affects line shape but not the flux/luminosity claims.
assumptions (4)
  • domain assumption The Bonanno-Malafarina-Panassiti metric (Eq. 2) is a valid physical description of collapse in asymptotic safety.
    The paper uses this metric as input without deriving or independently testing it; the regularity claim from [37] is not supported by the metric's Kretschmann scalar, which diverges at r=0.
  • domain assumption The accretion disk is geometrically thin, optically thick, Keplerian, and described by the Novikov-Thorne model with zero torque at the inner edge.
    Flux and luminosity formulas (Eqs. 29-31) rely on this standard model; real disks may have magnetic stresses or different inner boundary conditions.
  • domain assumption The inner edge of the emitting disk is at the ISCO and emissivity follows a power law with index α.
    Iron line simulations (Sec. V) assume r_in = r_isco and I_e ∝ r^{-α}; these choices determine the line shape, and the paper notes the actual disk geometry is unknown.
  • ad hoc to paper For ξ/M0^2 in (0.67,1.05), the inner stable region does not contribute to the emitted flux.
    The paper explicitly excludes this region from its flux calculation (Sec. IV) but still presents the brightening trend as a general result.

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Pith. "Pith review of Observational properties of regular black holes in Asymptotic Safety." pith.science (2026). https://pith.science/paper/H32QQ2DZ

@misc{pith2026250412072,
  author       = {Pith},
  title        = {Pith review of: Observational properties of regular black holes in Asymptotic Safety},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/H32QQ2DZ}},
  note         = {Machine review of arXiv:2504.12072}
}
abstract

We consider the observational properties of a spherically symmetric, static regular black hole within the framework of asymptotic safety (AS) as proposed by Bonanno et al. The metric resembles the Schwarzschild solution in the classical limit. The departure from Schwarzschild at small scales is controlled by a single free parameter related to the ultraviolet (UV) cutoff of the theory. We investigated null and time-like geodesics around the AS metric, including circular orbits, photon rings and lensing effects. In particular we focused on the optical properties of thin accretion disks in the equatorial plane of the object and compared them with those of accretion disks in the Schwarzschild metric. We found that the radiation flux, luminosity, and efficiency of the accretion disk increase with the value of the free parameter. Using a spacetime generic open-source relativistic ray-tracing code, we simulate the K$\alpha$ iron line profiles emitted by the disk and analyze their deviation from that of the Schwarzschild geometry.

Figures

Figures reproduced from arXiv: 2504.12072 by the authors.

Figure 1
Figure 1. FIG. 1: The solid black line shows the horizon radius [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 3
Figure 3. shows the dependence of the deflection angle on the inverse of the impact parameter 1/b for Schwarzschild and the ASBH (with ξ/M2 0 = 0.3, 2/3). The vertical dot￾ted lines in [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 5
Figure 5. FIG. 5: The dash-dotted line represents the AS innermost [PITH_FULL_IMAGE:figures/full_fig_p005_5.png] view at source ↗
Figures from the paper (4 more)
Figure 6
Figure 6. Figure 6: FIG. 6: Radiative Flux [PITH_FULL_IMAGE:figures/full_fig_p006_6.png]
Figure 9
Figure 9. Figure 9: FIG. 9: The efficiency of conversion of matter into radiated [PITH_FULL_IMAGE:figures/full_fig_p007_9.png]
Figure 8
Figure 8. Figure 8: FIG. 8: Spectral Luminosity of the thin accretion disk as a [PITH_FULL_IMAGE:figures/full_fig_p007_8.png]
Figure 10
Figure 10. Figure 10: FIG. 10: Simulation of the K [PITH_FULL_IMAGE:figures/full_fig_p009_10.png]

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