REVIEW 4 major objections 4 minor 2 cited by
Regular Black Hole from gravitational collapse of dust and radiation
T0 review · 4 major / 4 minor · reviewed 2026-08-10 · deepseek-v4-flash
Pith's one-line read A center-directed energy exchange can make collapsing dust end in a regular black hole
desk verdict The idea has a kernel, but the worked example fails its own equations and the regular core runs on negative energy. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
The load-bearing mechanism is the energy-exchange term $\beta(r)$ inserted into the separate continuity equations for dust and radiation. Taking $\beta(r)=8/3 - a r$ makes the exchange intensity toward the center, and this particular profile makes both component densities separately finite at $r=0$ once the integration constant $c_1$ is fixed by condition (31). Condition (34) then fixes $M_0$ so the mass function vanishes at the center, which turns the curvature scalars finite. The interaction profile is what converts a singular collapse endpoint into a regular one.
What would settle it
Evaluate the junction conditions between the interior metric (33) and the exterior metrics (11) or (19) at a radius $R$; if no physically acceptable matching exists, or if the central density must be nonnegative and it is not, the regular black hole model does not survive.
Extended reading notes
Core claim
The paper's central claim is that the interior of a collapsing cloud made of dust and radiation can have a regular center if the two components exchange energy through the interaction law $\beta(r)=8/3 - a r$, with the exchange strengthening as $r\to 0$. The resulting mass function, $M(v,r)=M_0[1 - a r/2 - (1 + a r/2)e^{-ar}]$, satisfies the regularity conditions when $c_1=-2\rho_{0r}/(3a^2)$ and $M_0=2\rho_{0r}/(3a^3)$: the mass tends to zero at the center, the density and pressure stay finite, and the Kretschmann scalar tends to $2M_0^2/(3a^6)$. The paper contrasts this with the no-interaction and constant-interaction cases, which leave a singular or only weakly singular center, and it notes the regular interior must be matched at some radius to an exterior solution before the whole spacetime can describe an observable black hole.
Load-bearing premise
The paper's conclusion rests on the assumed interaction profile $\beta(r)=8/3 - a r$ being a legitimate description of the matter, and on the interior solution being matchable to an exterior collapse solution at some radius.
Editorial extensions
If this is right
- If the claim is correct, a dust-and-radiation cloud with a center-directed energy exchange can end in a black hole whose center is regular rather than singular.
- The regularity conditions identified in the paper give later models a concrete target: central mass zero, finite central density, finite central pressure.
- The interior solution alone cannot predict black hole shadows or quasi-normal modes, so observable tests would have to use the matched exterior solution.
- In the period before horizons form, the central region may be visible to outside observers, so the model leaves open an observational signature from inside the collapsing cloud.
Reading between the lines
- A natural extension is to test whether other interaction profiles with $\beta'<0$ also yield a regular center; if they do, the mechanism is generic rather than an artifact of the chosen linear profile.
- The parameter $a(v)$ sets the length scale of the regular core; connecting it to a physical conversion rate between dust and radiation would turn the model into a quantitative prediction.
- Because the central total density in the explicit example is finite but negative, the model also raises the question of which effective energy conditions a physically acceptable regular core should satisfy.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper studies spherically symmetric gravitational collapse of a two-component fluid (dust and radiation) in generalized Vaidya coordinates. It first treats the non-interacting case and a constant-interaction case, obtaining the mass functions (11) and (19), and notes that these produce a singular center. It then proposes an r-dependent energy exchange β(r)=8/3−ar between dust and radiation, leading to an interior mass function M(v,r)=M0[1−ar/2−(1+ar/2)e^{-ar}]. With the choices c1=−2ρ0r/(3a^2) and M0=2ρ0r/(3a^3), the central densities are finite and the mass function vanishes at r=0; the paper claims this gives a regular black hole, while acknowledging that the solution covers only the inner region and must be matched to an exterior solution.
Significance. If the construction were physically viable, it would be a useful explicit example of a time-dependent regular black hole sourced by familiar matter with a phenomenological interaction. The derivation is self-contained and gives closed-form densities and mass functions. However, the explicit example in Section IV is not a positive-energy dust-radiation model: condition (34) forces negative mass and negative energy density in the core, and the required matching to a positive-mass exterior is not performed. The paper therefore does not establish its announced claim that collapse of ordinary matter can form a regular center, and its significance as a physical model is currently limited to a local, energy-condition-violating patch.
major comments (4)
- [Section IV, Eq. (25) vs. Eq. (30)] The sign of the interaction term in Eq. (25) is opposite to the sign in Eq. (17) and opposite to what the solution (30) actually satisfies. With Eq. (25) as printed (and with the implicit 1/r factors), the radiation equation gives ρ_r'/ρ_r = −8/(3r) − β/r, which for β=8/3−ar yields ρ_r ∝ e^{ar} r^{-16/3}, not ρ0r e^{-ar}. Thus (30) does not solve (25); the solved densities correspond to Eq. (17) with β=8/3−ar. This sign inconsistency must be fixed before the construction can be evaluated.
- [Section IV, Eqs. (32), (34), (35)] The regularity condition (34) forces negative energy in the core. For M0=2ρ0r/(3a^3)>0, differentiating (35) gives d(M/M0)/dr = (a/2)[(1+ar)e^{-ar}−1] < 0 for all r>0, so M(v,r)<0 for every r>0. Equations (30) and (32) give ρ_r(0)=ρ0r, ρ_m(0)=−4ρ0r/3, and ρ(0)=−ρ0r/3. If ρ0r>0, the dust and total densities are negative; if ρ0r<0, the radiation density is negative. Hence no choice of sign of ρ0r yields a positive-energy dust-plus-radiation source, and the weak energy condition is violated by at least one component. The announced model of ordinary-matter collapse is therefore not supported by the example.
- [Section IV, final paragraph] The matching to the exterior solutions (11) or (19) is asserted but never carried out. Since M(v,r) in (35) is strictly negative for r>0 while the exterior solutions are constructed as positive-mass black holes, a continuous junction with positive-energy matter cannot be achieved without a shell carrying negative energy. Without an explicit junction analysis, the paper establishes only a local regular interior patch, not a global regular black hole spacetime.
- [Section IV, Eq. (36)] The stated central limit of the Kretschmann scalar has incorrect dimensions. With M0 of dimension length and a of dimension inverse length, M0^2/a^6 has dimension L^8, whereas K must have dimension L^{-4}. The regularity claim only requires finiteness, but the value printed in (36) should be recomputed; the curvature scale is set by M0^2 a^6 or an equivalent combination.
minor comments (4)
- [Eqs. (7), (8), (17), (25)] These continuity equations are dimensionally inconsistent as written because the non-derivative terms lack factors of 1/r. The stated power-law solutions (9), (18), and (30) require the standard forms such as ρ_d' + 2ρ_d/r = 0; please correct all such equations.
- [Section IV] There are unresolved equation references '(??)' immediately before Eqs. (29) and (30); these should be actual equation numbers.
- [Eq. (24)] Equation (24) is written with an unexplained arrow and should be presented as an algebraic equation; the claim that it has a positive root in (0,1) under the stated inequality needs a brief justification.
- [Throughout] There are typos, including 'r adiation' in the title, and 'explycit', 'apsent', 'simplisity', and 'carvature' in the text.
Circularity Check
No significant circularity: the regular-center solution is an openly constructed example with integration constants tuned to the stated regularity conditions, and the paper's self-citations are background only.
full rationale
The paper's central example is self-contained and openly constructive. The regularity criteria are stated in Sec. II as limits on M, rho, and P that make the curvature invariants (12)-(14) finite at r=0. In Sec. IVA the author chooses beta(r)=8/3-ar and then fixes the integration constants via (31) and (34) precisely so that those limits hold. This is not a hidden equivalence: the mass function (35) is the integral of the chosen density, and the constants are not fitted to an external dataset or to a prior result that itself assumes regularity. The paper explicitly labels the result an 'explicit example' and concedes that (33) covers only the inner region and must be matched to (11) or (19), so the claim is limited to existence of a locally regular core, not a complete collapse prediction. The self-citations (refs. [15], [19], [22]) provide background on Hagedorn fluids, polytropic Vaidya collapse, and naked singularity formation; none is load-bearing for the derivation of (35). The negative-energy issue raised by a skeptical reader is a physical correctness concern (weak energy condition violation and matching difficulty), not a circularity of the derivation. Therefore no circular step is exhibited, and the paper receives a low score reflecting only minor non-load-bearing self-citation.
Assumptions & free parameters
free parameters (3)
- a(v)
- rho_0r(v)
- M0(v)
assumptions (4)
- domain assumption The collapsing cloud is described by the generalized Vaidya metric (1) in Eddington-Finkelstein coordinates.
- domain assumption The matter content is only dust with P_d=0 and radiation with P_r=rho_r/3, with total energy-momentum conservation but separate components not conserved.
- ad hoc to paper The interaction rate beta(r)=8/3-a r is chosen so that the radiation density becomes rho_r=rho_0r e^{-ar}.
- ad hoc to paper The inner solution (33) can be matched to an exterior solution (11) or (19) at some radius R.
invented entities (1)
-
Radial energy-exchange interaction beta(r)
Cite this review
Pith. "Pith review of Regular Black Hole from gravitational collapse of dust and radiation." pith.science (2026). https://pith.science/paper/Y5UOLFKJ
@misc{pith2026250113739,
author = {Pith},
title = {Pith review of: Regular Black Hole from gravitational collapse of dust and radiation},
year = {2026},
howpublished = {\url{https://pith.science/paper/Y5UOLFKJ}},
note = {Machine review of arXiv:2501.13739}
}
read the original abstract
A black hole is the end state of the gravitational collapse of massive stars. However, a typical black hole contains a singularity and to avoid singularity formation we have to violate a strong energy condition that states that gravity must attract. The nature of the matter that prevents the singularity formation is still unknown. In this paper, we offer a simple model of gravitational collapse of dust and radiation. In the simplest case, such a model leads to a singular black hole. However, if we assume an energy exchange between dust and radiation, which increases towards the center of the collapsing cloud, then it becomes possible to construct a model of a regular black hole. We identify the conditions under which a regular center is possible and also give an explicit example of how such an interaction leads to a regular center.
Forward citations
Cited by 2 Pith papers
-
Regular Black Hole Formation and Gamma-Ray Burst from Matter Conversion
The formation of a regular black hole could release gamma-ray-burst-scale energy only if its singularity-avoiding core is a weak perturbation of Schwarzschild.
-
Formation of regular black hole from baryonic matter
A family of regular black hole collapse solutions is built by imposing a de Sitter core and matching to a Husain exterior; the shadow radius grows with the barotropic parameter alpha.
Reference graph
Works this paper leans on
-
[1]
This limit always leads to gravitationally weak singulari ty - important property because the solution ( 11) always lead to gravitationally strong singularity [ 23–25]. One should also note, that when gravitational collapse st arts at v = 0 singularity is apsent and the region near this regular core might be visib le by faraway observer. To prove this sta...
-
[2]
The Event Horizon Telescope Collaboration, firstM87 Eve nt Horizon Telescope results. I. The shadow of the supermass ive black hole, Astrophys. J. Lett. 875 (2019)L1
work page 2019
-
[3]
Akiyama, K. et al. [Event Horizon Telescope Collaborati on]. First Sagittarius A ∗ Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole in the Center of the Milky Way. Astrophys. J. Lett. 2022, 930, L12
work page 2022
-
[4]
Penrose, Gravitational Collapse and Space-Time Sing ularities
R. Penrose, Gravitational Collapse and Space-Time Sing ularities. Phys. Rev. Lett. 14, 57 (1965)
work page 1965
-
[5]
S. Ansoldi, Spherical black holes with regular center: a review of existing models including a recent realization wi th Gaussian sources. [ arXiv:0802.0330 [gr-qc]]
-
[6]
C. Lan, H. Yang, Y. Guo and Y. G. Miao, Int. J. Theor. Phys. 62 (2023) no.9, 202 [ arXiv:2303.11696 [gr-qc]]
arXiv 2023
-
[7]
A. Bonanno, D. Malafarina and A. Panassiti, Phys. Rev. Le tt. 132 (2024) no.3, 031401 [ arXiv:2308.10890 [gr-qc]]
arXiv 2024
-
[8]
K. A. Bronnikov, Phys. Rev. D 63 (2001), 044005 [ arXiv:gr-qc/0006014 [gr-qc]]
arXiv 2001
Show all 28 references
-
[9]
Konoplich, S.G
R.V. Konoplich, S.G. Rubin, A.S. Sakharov, M.Yu. Khlopo v, FORMATION OF BLACK HOLES IN FIRST-ORDER PHASE TRANSITIONS AS A COSMOLOGICAL TEST OF SYMMETRY-BREAKING ME CHANISMS. Phys.Atom.Nucl.62:1593- 1600,1999, Yad.Fiz.62:1705-1713,1999
1999
-
[10]
Khlopov, R.V
M.Yu. Khlopov, R.V. Konoplich, S.G. Rubin, A.S. Sakharo v, FIRST-ORDER PHASE TRANSITIONS AS A SOURCE OF BLACK HOLES IN THE EARLY UNIVERSE. Grav.Cosmol.6:153-156,2000
2000
-
[11]
E. B. Gliner, Algebraic Properties of the Energy-momen tum Tensor and Vacuum-like States of Matter, Sov. Phys. JETP 22 (1966) 378. 7
1966
-
[12]
A. D. Sakharov, The initial stage of an expanding Univer se and the appearance of a nonuniform distribution of matter , Sov. Phys. JETP 22 (1966) 241
1966
-
[13]
Bardeen, Conference Proceedings in GR5, Tiflis, U.S
J. Bardeen, Conference Proceedings in GR5, Tiflis, U.S. S.R., (1968)
1968
-
[14]
S. A. Hayward, Phys. Rev. Lett. 96 (2006), 031103 [ arXiv:gr-qc/0506126 [gr-qc]]
2006 arXiv
-
[15]
Dymnikova, ”Vacuum nonsingular black hole”
I. Dymnikova, ”Vacuum nonsingular black hole”. Genera l Relativity and Gravitation. 24, No. 3, 235-243 (1992)
1992
-
[16]
Vertogradov, A
V. Vertogradov, A. ¨Ovg¨ un, Exact Regular Black Hole Solutions with de Sitter Co res and Hagedorn Fluid. Class. Quantum Grav. 42 025024 (2025) [ arXiv:2408.02699 [gr-qc]]
2025 arXiv
-
[17]
Oppenheimer, H.Snyder, On Continued Gravitation al Contraction
J.R. Oppenheimer, H.Snyder, On Continued Gravitation al Contraction. Phys. Rev. 56, 455-459 (1939)
1939
-
[18]
Joshi Gravitational collapse and spacetime s ingularities
Pankaj S. Joshi Gravitational collapse and spacetime s ingularities. Cambridge University Press. 2007.p.273
2007
-
[19]
Joshi, D
Pankaj S. Joshi, D. Malafarina, ”Recent development in gravitational collapse and spacetime singularitits”. Int . J. Mod. Phys. D, 20 2641 (2011)
2011
-
[20]
Vertogradov, The generalized Vaidya spacetime with polytropic equation of state
V. Vertogradov, The generalized Vaidya spacetime with polytropic equation of state. General Relativity and Gravi tation (2024) 56:59
2024
-
[21]
Gravitat ional collapse of generalized Vaidya spacetime
Mkenyeleye, M.D.; Goswami, R.; Maharaj, S.D. Gravitat ional collapse of generalized Vaidya spacetime. Phys. Rev. D 2015, 92, 024041
2015
-
[22]
Husain, Exact solutions for null fluid collapse
V. Husain, Exact solutions for null fluid collapse. Phys. Rev. D 1996, 53, R1759, [ arXiv:gr-qc/9511011]
1996 arXiv
-
[23]
Vertogradov, Naked singularity formation in genera lized Vaidya space-time
V. Vertogradov, Naked singularity formation in genera lized Vaidya space-time. Grav. Cosmol. 2016, 22, 220–223
2016
-
[24]
F.J.Tipler, Phys. Lett. A 64, 8 (1977)
1977
-
[25]
Nolan Phys
Brien C. Nolan Phys. Rev. D 60, 024014
-
[26]
C. J. S Clarke and A. Krolak, J. Geom. Phy. 12 127 (1985)
1985
-
[27]
Chakrabarti, P.S
S.K. Chakrabarti, P.S. Joshi, Naked Singularities as P ossible Candidates for Gamma-ray Bursters, [ arXiv:hep-th/9208060]
-
[28]
T. Harko. Gravitational collapse of a Hagedorn fluid in V aidya geometry, Phys.Rev. D68 (2003) 064005
2003
Reviewed August 10, 2026 · model on record in the stance chip above.
Discussion (0). Continue with ORCID to comment.