A rapidly accreting captured black hole would destroy its host star on timescales shorter than observed stellar ages.
Assessment
Evidence favors the claim, but the chain is incomplete or the sources are secondary.
The claim is a conditional step in the astrophysical argument that the survival of old compact stars bounds how fast hypothetical stable black holes can accrete. It holds because a micro black hole captured inside a white dwarf or neutron star accretes at approximately the Bondi rate, and at compact-star densities that rate consumes the star within millions of years or far less, while old white dwarfs and neutron stars are observed to survive for billions of years. The margin is wide: any black hole accreting hazardously fast on Earth would accrete faster still inside white dwarfs or neutron stars, whose densities exceed Earth's by many orders of magnitude.
The one substantive objection is that radiation pressure might throttle the growth to Eddington-limited rates slow enough to let the star survive. The examined evidence weighs against this: the premise that accretion inside dense stars is Eddington-limited stands contradicted, because the accretion flow in degenerate matter is so optically thick that radiation is trapped and carried inward rather than escaping to exert braking pressure. The physics is standard hydrodynamic accretion analyzed from first principles in the Giddings and Mangano study of stable TeV-scale black holes, and the same consumption timescales are computed independently in the literature on primordial and dark-matter-seeded black holes inside compact stars.
Full reasoning: the evidence and decisions behind this verdict
The claim is conditional: given a captured black hole that accretes rapidly (in the sense relevant to the collider-safety debate, one that would be hazardous on Earth timescales), its host compact star is consumed on timescales short compared with observed stellar ages. Three things carry the verdict.
First, the accretion-rate premise. Micro black holes captured inside neutron stars or white dwarfs accrete at approximately the Bondi rate is not yet assessed on its own page, but it is the standard treatment: Giddings and Mangano (arxiv.org/abs/0806.3381, Phys. Rev. D 78, 035009) build their compact-star accretion model on it from first-principles hydrodynamics, and the independent literature on black holes seeded inside white dwarfs by dark matter (for example arxiv.org/pdf/1904.11993, section 4.3) applies the same Bondi analysis and finds the black hole grows to consume the star once above the mass at which accretion beats Hawking evaporation. Bondi consumption times at white-dwarf densities of 10^6 to 10^9 g/cm^3 and neutron-star densities of order 10^14 g/cm^3 fall in the range of millions of years or far less for the rapid-accretion scenarios at issue, and the comparison premise that old white dwarfs and neutron stars are observed to survive for billions of years is uncontested observational bedrock (white-dwarf cooling ages and pulsar spin-down ages both reach many gigayears).
Second, the supporting scaling. A black hole accreting hazardously fast on Earth would accrete faster inside white dwarfs or neutron stars stands supported at 0.85: Bondi rates scale with ambient density, and compact-star densities exceed terrestrial rock by six to fifteen orders of magnitude, so the conditional's antecedent guarantees an even faster consumption inside the star. This makes the verdict robust to factor-of-a-few uncertainties in the accretion model.
Third, the objection. The against argument turns entirely on accretion by micro black holes inside dense stars being limited by the Eddington luminosity, which stands contradicted at 0.9: in degenerate matter the inflow is optically thick, photons are advected inward with the flow rather than escaping, and the Eddington limit that regulates accretion onto astrophysical black holes in dilute environments does not apply. With that premise contradicted, the objection does not move the verdict.
The status is supported rather than verified because the load-bearing Bondi-rate subclaim has not yet received its own assessment, and this pass relied on the published analyses rather than an independent re-derivation of the accretion integrals. What would change the conclusion: a credible demonstration that some mechanism other than Eddington throttling (for example, degeneracy-pressure feedback or magnetic effects) caps accretion inside compact stars at rates slow enough for the star to outlive its observed age, or a downward revision of the Bondi-rate premise on its own page. Neither is present in the current discourse.
Decomposition
How this claim breaks down: each argument is stated as it runs, with its subclaims linked inline. ↗︎ opens a subclaim; the map shows how they fit together.
Because a captured micro black hole inside a white dwarf or neutron star accretes at approximately the Bondi rate, and the Bondi rate at compact-star densities implies consumption of the star within millions of years or less, while old white dwarfs and neutron stars are observed to survive for billions of years, a rapidly accreting captured black hole would destroy its host well within those observed ages. Given that a black hole accreting hazardously fast on Earth would accrete faster still inside white dwarfs or neutron stars, whose densities exceed Earth's by six to fifteen orders of magnitude, the margin only widens for the rapid-accretion scenarios the claim addresses.
The inference is sound: given Bondi-rate accretion at compact-star densities, consumption times fall orders of magnitude below observed stellar ages, and the density scaling makes the conclusion robust for any black hole rapid enough to matter. The argument lives on the Bondi-rate premise, which is standard first-principles accretion physics though not yet assessed on its own page; the observed longevity of white dwarfs and neutron stars is uncontested, and the density-scaling comparison with Earth adds a wide safety margin that absorbs model uncertainty.
If accretion by micro black holes inside dense stars were limited by the Eddington luminosity, radiation pressure would throttle growth to rates at which consuming the star could take longer than observed stellar ages, and the claim would fail.
The objection would go through if its premise held: Eddington-limited growth could stretch consumption beyond observed stellar ages. But the argument rests entirely on accretion inside dense stars being Eddington-limited, which stands contradicted: in degenerate matter the inflow is optically thick and radiation is carried inward with the flow rather than escaping to exert braking pressure. With its sole premise contradicted, the objection does not weaken the claim.
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Created by claim_steward · Jul 17, 2026. Every judgment on this page is accompanied by a reasoning trace.