Primordial Black Holes with QCD Color Charge

David I. Kaiser; Elba Alonso-Monsalve

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Primordial Black Holes with QCD Color Charge

Elba Alonso-Monsalve, David I. Kaiser

High Energy Physics - Phenomenology · Submitted 25 Oct 2023

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We describe a realistic mechanism whereby black holes with significant QCD color charge could have formed during the early universe.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 3,551 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.12 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.18 · compares with prior results 0.06 · mentions code or data availability 0.01.

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We describe a realistic mechanism whereby black holes with significant QCD color charge could have formed during the early universe. Primordial black holes (PBHs) could make up a significant fraction of the dark matter if they formed well before the QCD confinement transition. Such PBHs would form by absorbing unconfined quarks and gluons, and hence could acquire a net color charge. We estimate the number of PBHs per Hubble volume with near-extremal color charge for various scenarios, and discuss possible phenomenological implications.

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What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We describe a realistic mechanism whereby black holes with significant QCD color charge could have formed during the early universe.	contribution 1.00	0.88	0.35	asserted 0.70
s1	Primordial black holes (PBHs) could make up a significant fraction of the dark matter if they formed well before the QCD confinement transition.	background 0.99	0.08	0.14	hedged possibility 1.00
s2	Such PBHs would form by absorbing unconfined quarks and gluons, and hence could acquire a net color charge.	method 0.46	0.16	0.16	hedged possibility 0.95
s3	We estimate the number of PBHs per Hubble volume with near-extremal color charge for various scenarios, and discuss possible phenomenological implications.	contribution 0.96	0.95	0.18	asserted 0.90

What kind of paper the classifier reports this is: theoretical result 1.00 · evidence from proof or derivation 0.45.

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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

We describe a realistic mechanism whereby black holes with significant QCD color charge could have formed during the early universe. Primordial black holes (PBHs) could make up a significant fraction of the dark matter if they formed well before the QCD confinement transition. Such PBHs would form by absorbing unconfined quarks and gluons, and hence could acquire a net color charge. We estimate the number of PBHs per Hubble volume with near-extremal color charge for various scenarios, and discuss possible phenomenological implications.

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References

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5 arXiv papers cite this in 7 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 6 sentences without a confident label

Cites it as background 1 paper

There are a numerous mechanisms to form PBHs based on an early matter era [ref] , modified gravity [ref] , scalar field instabilities [ref] , collapse of cosmic strings [ref] and domain walls [ref] , phase transitions [ref] , bubble collisions [ref] , standard model Higgs instability [ref] and from unconfined quarks and gluons [ref] .

Cosmic Whispers of the Early Universe: Gravitational Waves and Dark Matter from Primordial Black Holes · Formation mechanisms · 0.85

What it cites · 100 sentences without a confident label

Uses the method or tool of 1 paper

We follow the background-field method as in Ref. [ref] , which allows us to choose the action of the gauge symmetry to act only on $a^c_μ$, so no explicit gauge-fixing terms or ghosts are required in $S_eff$.

The Quark-Gluon Plasma: Collective Dynamics and Hard Thermal Loops · Introduction · 1.00

Uses data or values from 4 papers

The universal scaling exponent $ν$ depends on the equation of state of the fluid that undergoes collapse; numerical studies show $ν= 0.36$ for a radiation fluid [ref] .

Primordial black hole formation in the radiative era: investigation of the critical nature of the collapse · Introduction · 0.95
The universal scaling exponent $ν$ depends on the equation of state of the fluid that undergoes collapse; numerical studies show $ν= 0.36$ for a radiation fluid [ref] .

Dynamics of Primordial Black Hole Formation · Introduction · 0.95
The universal scaling exponent $ν$ depends on the equation of state of the fluid that undergoes collapse; numerical studies show $ν= 0.36$ for a radiation fluid [ref] .

Observation of critical phenomena and self-similarity in the gravitational collapse of radiation fluid · Introduction · 0.95

Cites as support 1 paper

First, the PBH's charge is strongly screened in the medium [ref] , reducing the probability of the PBH preferentially absorbing compensating charges.

Debye Screening of Non-Abelian Plasmas in Curved Spacetimes · Introduction · 0.99

Cites as background 21 papers

(For reviews, see Refs. [ref] .) This holds even within an expanding Friedmann-Lemaître-Robertson-Walker (FLRW) spacetime, given the large hierarchy of scales $λ_D≪H^-1$.

Color Screening in Quantum Chromodynamics · Introduction · 0.95
(For reviews, see Refs. [ref] .) This holds even within an expanding Friedmann-Lemaître-Robertson-Walker (FLRW) spacetime, given the large hierarchy of scales $λ_D≪H^-1$.

Semi-classical transport theory for non-Abelian plasmas · Introduction · 0.95
(For reviews, see Refs. [ref] .) This holds even within an expanding Friedmann-Lemaître-Robertson-Walker (FLRW) spacetime, given the large hierarchy of scales $λ_D≪H^-1$.

The Quark-Gluon Plasma: Collective Dynamics and Hard Thermal Loops · Introduction · 0.95

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