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arxiv: 2605.10587 · v1 · submitted 2026-05-11 · 🌌 astro-ph.HE · gr-qc· hep-ph

Recognition: no theorem link

Astrons: Reissner-Nordstr\"om Primordial Naked Singularities

Claudio Corian\`o , Paul H. Frampton , Leonardo Torcellini
Authors on Pith no claims yet

Pith reviewed 2026-05-12 04:30 UTC · model grok-4.3

classification 🌌 astro-ph.HE gr-qchep-ph
keywords astronsReissner-Nordströmprimordial naked singularitiescharge saturationplasma screeningearly universe structurescosmological accelerationdark seeds
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The pith

A population of primordial ultra-massive charged compact objects is subject to tight physical constraints and does not produce late-time cosmic acceleration in the standard model.

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

The paper proposes and constrains astrons as primordial ultra-massive electrically charged compact objects whose exterior is described by the Reissner-Nordström geometry. It integrates limits from charge generation via accretion, saturation in ionized media, screening by intergalactic plasma, gravitational lensing, and the cosmological evolution of their energy density. If the scenario holds, these objects could act as dark seeds explaining early structures seen in observations without being directly luminous at high redshift. The analysis reveals that standard accretion produces charges well below phenomenological targets, plasma screening is a major hurdle, and the interaction energy of the population falls off as the inverse fourth power of the scale factor, yielding only a transitory effect on expansion rather than sustained acceleration.

Core claim

Astrons are primordial, ultra-massive, electrically charged compact objects whose geometry is Reissner-Nordström. Constraints arise from charge saturation during formation, persistence against screening in plasma, and the scaling of their mutual interaction energy, which behaves as a^{-4} in homogeneous cosmology. This prevents the population from driving asymptotic late-time acceleration, though they might seed early cosmic structures as dark components rather than observed luminous objects.

What carries the argument

The Reissner-Nordström geometry of highly charged compact objects combined with the homogeneous FLRW scaling of their interaction energy.

Load-bearing premise

That ordinary accretion saturation applies to these ultra-massive objects and that the interaction energy of the charged population scales exactly as a^{-4} in the homogeneous FLRW description without additional contributions from inhomogeneities.

What would settle it

Observation of a compact object with charge significantly exceeding the saturation value from standard accretion, or cosmological measurements indicating a sustained acceleration phase linked to a charged component rather than a transitory one.

Figures

Figures reproduced from arXiv: 2605.10587 by Claudio Corian\`o, Leonardo Torcellini, Paul H. Frampton.

Figure 1
Figure 1. Figure 1: Representative charge scales as functions of mass. The figure summarizes the separation between ordinary accretion-saturation branches and the large [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: RN characteristic radii as functions of Ξ. The outer horizon ceases to exist at Ξ = 1, while the photon sphere persists only to Ξ = 9/8. The distinction between these two thresholds is essential for the interpretation of horizonless but still strongly lensing configurations. It therefore contributes positively to ρ + 3p and cannot act as a cosmological constant. This result is important because it separate… view at source ↗
Figure 3
Figure 3. Figure 3: Screened lattice diagnostic for a Yukawa-regulated inter-astron interaction. If the screening length is shorter than the inter-source spacing, the collective [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
read the original abstract

We summarize a set of constraints on a proposed population of primordial, ultra-massive, electrically charged compact objects, which we call astrons. The analysis combines charge generation, charge saturation, persistence of the charge in an ionized medium, screening by the intergalactic plasma, the Reissner--Nordstr\"om geometry of highly charged compact objects, lensing, and the cosmological implications of a sparse charged population. We also discuss the possible relation to the early structures revealed by the James Webb Space Telescope: if astrons are relevant there, they would be primordial dark seeds rather than luminous objects directly observed at high redshift. The resulting scenario is sharply constrained. Ordinary accretion saturation gives charges far below the large-charge phenomenological benchmark, screening is a serious plasma-physics issue, and a large charge can place the exterior geometry deep in the super-extremal regime. As expected at the level of a homogeneous Friedmann--Lema\^{\i}tre--Robertson--Walker (FLRW) description, the interaction energy of a population of charged objects scales as \(a^{-4}\), so the simplest perfect-fluid reduction does not generate asymptotically late-time acceleration; any acceleration era tied to that homogeneous component can only be transitory. The astron scenario should be regarded as a constrained framework whose viability depends on plasma physics and on a cosmological treatment beyond the homogeneous approximation.

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

2 major / 2 minor

Summary. The manuscript proposes a population of primordial ultra-massive electrically charged compact objects termed 'astrons,' modeled as Reissner-Nordström naked singularities. It presents a synthesis of constraints from charge generation, accretion saturation, persistence in ionized media, plasma screening, RN geometry (including super-extremal cases), lensing, and cosmological evolution. In the homogeneous FLRW framework, the charged population's interaction energy is shown to scale as a^{-4}, implying that the simplest perfect-fluid description does not produce late-time acceleration. The scenario is described as sharply constrained, with potential relevance to JWST early structures only if astrons serve as dark seeds. Viability is said to depend on detailed plasma physics and extensions beyond homogeneous cosmology.

Significance. If the results hold, this work is significant in providing a constrained framework for primordial charged singularities, correctly noting that homogeneous scaling precludes asymptotic acceleration and identifying plasma screening as a key obstacle. The integration of general relativity, plasma physics, and cosmology is a strength, offering a balanced view that avoids overclaiming observational links to JWST data. No machine-checked proofs or code are included, but the emphasis on falsifiable elements like lensing and the call for non-homogeneous treatments adds value. The assessment highlights gaps that future work must address.

major comments (2)
  1. [Cosmological implications] Cosmological implications section: The statement that the interaction energy of the charged population scales as a^{-4} in homogeneous FLRW (leading to no asymptotic acceleration) is central to the no-acceleration claim. This derives from standard perfect-fluid treatment, but the manuscript notes potential modifications from plasma screening and inhomogeneities without providing an explicit calculation of screened Coulomb energy in expanding spacetime or metric back-reaction. This approximation is load-bearing for the conclusion that any acceleration is only transitory.
  2. [Charge saturation] Charge saturation section: The claim that ordinary accretion saturation produces charges far below the large-charge phenomenological benchmark is used to argue the scenario is sharply constrained. However, the text does not include the specific derivation or numerical comparison to the benchmark, making it difficult to verify the extent of the constraint and its implications for the overall model.
minor comments (2)
  1. [Abstract] The term 'astrons' is introduced without immediate definition or context; adding a brief explanatory phrase would improve accessibility for readers.
  2. [Notation] The use of a for the scale factor in a^{-4} is clear but should be explicitly linked to the FLRW metric definition in the cosmological section for consistency.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We address each of the major comments below and have made revisions to the manuscript where appropriate.

read point-by-point responses

  1. Referee: [Cosmological implications] Cosmological implications section: The statement that the interaction energy of the charged population scales as a^{-4} in homogeneous FLRW (leading to no asymptotic acceleration) is central to the no-acceleration claim. This derives from standard perfect-fluid treatment, but the manuscript notes potential modifications from plasma screening and inhomogeneities without providing an explicit calculation of screened Coulomb energy in expanding spacetime or metric back-reaction. This approximation is load-bearing for the conclusion that any acceleration is only transitory.

    Authors: We appreciate the referee's focus on this key aspect. The a^{-4} scaling arises directly from treating the charged population as a perfect fluid in the homogeneous FLRW metric, where the Coulomb interaction energy density scales identically to radiation. This is a standard result in charged cosmological models. The manuscript explicitly qualifies this as holding 'at the level of a homogeneous Friedmann–Lemaître–Robertson–Walker (FLRW) description' and notes that plasma screening and inhomogeneities could modify the behavior. We agree that a full explicit calculation of the screened Coulomb energy in an expanding spacetime, incorporating metric back-reaction, is not included, as it would require a detailed non-homogeneous treatment beyond the paper's scope. We have revised the text to more clearly highlight this as a limitation of the homogeneous approximation and to reinforce the call for future work on non-homogeneous cosmology. revision: partial

  2. Referee: [Charge saturation] Charge saturation section: The claim that ordinary accretion saturation produces charges far below the large-charge phenomenological benchmark is used to argue the scenario is sharply constrained. However, the text does not include the specific derivation or numerical comparison to the benchmark, making it difficult to verify the extent of the constraint and its implications for the overall model.

    Authors: We thank the referee for this observation. To improve verifiability, we have added the explicit derivation of the saturation charge from standard accretion processes in the revised manuscript. This includes the relevant equations and a numerical comparison demonstrating that the saturated charges are significantly below the large-charge benchmark (by several orders of magnitude), thereby strengthening the argument that the scenario is sharply constrained by charge saturation. revision: yes

Circularity Check

0 steps flagged

No circularity: standard FLRW scaling applied without reduction to fitted inputs or self-citations.

full rationale

The paper states that interaction energy scales as a^{-4} 'as expected at the level of a homogeneous FLRW description' and concludes that the perfect-fluid reduction yields no asymptotic late-time acceleration. This follows directly from standard cosmological scaling (number density ∝ a^{-3}, Coulomb energy ∝ a^{-1}) applied to charged objects treated as a perfect fluid; it is not derived from or equivalent to any paper-specific ansatz, fit, or self-citation. Charge saturation is compared against an external 'large-charge phenomenological benchmark' without claiming the benchmark itself as a derived prediction. The final assessment that viability depends on plasma physics and inhomogeneous cosmology is presented as an open constraint rather than a closed derivation. No load-bearing step reduces by construction to the paper's own inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 1 invented entities

The framework rests on standard general relativity for RN geometry and FLRW cosmology, with the new label 'astrons' as the main addition without independent evidence.

axioms (2)
  • standard math Reissner-Nordström geometry describes the exterior of highly charged compact objects
    Invoked for lensing and super-extremal regime analysis.
  • domain assumption Homogeneous FLRW metric for cosmological evolution
    Used to derive a^{-4} scaling of interaction energy.
invented entities (1)
  • astrons no independent evidence
    purpose: Primordial ultra-massive electrically charged compact objects as naked singularities
    New term for the proposed population; no falsifiable prediction or independent evidence provided.

pith-pipeline@v0.9.0 · 5556 in / 1345 out tokens · 41163 ms · 2026-05-12T04:30:09.357230+00:00 · methodology

discussion (0)

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