Survival of white dwarfs and neutron stars constrains TeV-scale black hole accretion rates.
Assessment
Evidence favors the claim, but the chain is incomplete or the sources are secondary.
The claim rests on the stellar-survival argument developed by Giddings and Mangano (2008): if stable TeV-scale black holes could be produced in particle collisions, cosmic rays striking white dwarfs and neutron stars over billions of years would have produced and deposited such black holes inside them, and the continued existence of very old white dwarfs and neutron stars therefore bounds how fast any captured black hole can accrete. The argument's most technically demanding link, that even neutral relativistic black holes would be stopped and captured inside these dense stars, is backed by peer-reviewed stopping-power calculations that were independently reproduced in 2016 and remain unrebutted, though the result is model-dependent on the assumed number of extra dimensions. The remaining links, that rapid accretion would destroy a host star quickly and that multi-billion-year-old white dwarfs and neutron stars are observed, are not seriously disputed.
The claim is deliberately modest: it asserts that stellar survival constrains accretion rates, not that it excludes any scenario outright. Known qualifications, such as magnetic screening of cosmic rays at neutron stars and the small sample of well-characterised white dwarfs anchoring that branch of the bound, weaken parts of the argument without removing the constraint, since the white-dwarf branch alone can carry it. No peer-reviewed physics challenge to the constraint itself has been published; full verification would require independent assessment of the accretion-timescale link, which has so far attracted little scrutiny precisely because it is not where the informed debate lies.
Full reasoning — evidence and decisions behind this verdict
Evidence base. The single source instance affirms the claim and comes from Giddings & Mangano, "Astrophysical implications of hypothetical stable TeV-scale black holes" (arXiv:0806.3381; Phys. Rev. D 78, 035009, 2008), a peer-reviewed primary analysis that became the basis of CERN's refined safety case. The same white-dwarf/neutron-star survival logic recurs independently in the primordial-black-hole constraint literature, corroborating the inference pattern.
How the subclaims weigh. The bound requires four links. (1) Cosmic rays striking these stars would produce such black holes within the scenario being constrained: assessed supported. (2) The capture crux, that black holes produced there would be stopped inside the stars whether charged or neutral, is now independently assessed as supported (charged black holes stop electromagnetically; the neutral-case gravitational stopping calculation of Giddings-Mangano was independently reproduced in 2016 and stands unrebutted, though it is model-dependent on the number of extra dimensions). This was previously the weakest point in the audit trail, held on the source's authority alone; its independent assessment strengthens the verdict and is reflected in a modest confidence increase. (3) Rapid accretion would destroy the host on timescales short against stellar ages: not yet independently assessed, but resting on accretion physics that is not seriously disputed. (4) Old white dwarfs and neutron stars are observed: uncontested. With the crux now assessed but the accretion-timescale link still resting on the peer-reviewed source, SUPPORTED rather than VERIFIED remains the honest reading.
Counter-considerations weighed. Magnetic screening of incident cosmic rays can weaken the neutron-star branch (acknowledged by Giddings and Mangano, emphasised by Johnson 2009), but the white-dwarf branch survives it and can carry the joint constraint alone. The white-dwarf bound rests on a handful of well-characterised stars, a quantifiable residual weakness rather than a refutation. The neighbouring contested claim that published risk analyses do not establish negligible catastrophic risk is a meta-level critique of safety argumentation and does not deny that stellar survival yields accretion-rate constraints. No peer-reviewed physics challenge to the constraint itself was found.
Credence 0.92 reflects that the claim is deliberately modest ("constrains", not "excludes"): it is very likely true as stated, with residual mass on the model-dependence of the neutral-capture calculation and the unassessed accretion-timescale link. A published refutation of the stopping-power calculation, or evidence that the accretion timescales in degenerate matter are far longer than stellar ages, would change this conclusion.
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 If TeV-scale black hole production is possible in particle collisions, cosmic rays striking white dwarfs or neutron stars would produce such black holes. and Stable microscopic black holes produced by cosmic rays striking white dwarfs or neutron stars would be stopped inside those stars, whether charged or neutral., any such black hole permitted by the scenario would accumulate inside these stars over their lifetimes. Given that A rapidly accreting captured black hole would destroy its host star on timescales shorter than observed stellar ages. while Old white dwarfs and neutron stars are observed to survive for billions of years, the accretion rate of such black holes must be low enough not to have destroyed the observed stars, which is the claimed constraint.
Provenance
Where this claim has been said, linked to its canonical form.
Their existence and observed properties place strong constraints on the possible production and accretion of such black holes.
Referring to white dwarfs and neutron stars, whose observed persistence bounds black hole accretion scenarios.
Assessment history
0 status changes over 2 assessments. full history →
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Created by extractor · Jul 17, 2026. Every judgment on this page is accompanied by a reasoning trace.