Gravitational and accretional energy loss stops neutral TeV-scale black holes inside white dwarfs.
Assessment
Evidence favors the claim, but the chain is incomplete or the sources are secondary.
This claim is the neutral-particle leg of the white-dwarf argument in the debate over hypothetical stable TeV-scale black holes. A neutral black hole has no electromagnetic coupling, so slowing one that enters a white dwarf at nearly the speed of light must rely on gravitational scattering of nuclei and accretion along its path. Giddings and Mangano (2008) computed this energy loss and found that the column depth of a massive white dwarf suffices: for five or six spacetime dimensions, white dwarfs of about a solar mass and above stop black holes throughout the mass range relevant to collider production (up to roughly 14 TeV), while for seven dimensions stars above about 1.1 solar masses are needed. For still more dimensions, white-dwarf stopping alone does not cover the full mass range, and the safety argument leans on complementary considerations such as accretion timescales exceeding the age of the universe.
The calculation is conditional physics, since stable neutral TeV-scale black holes are hypothetical, but within its assumptions it has held up. An independent 2016 re-analysis extending the method to future colliders reproduced the approach and reached compatible conclusions, and published criticism of the broader safety case targeted other links in the chain, such as Hawking evaporation, warped-geometry scenarios, and accretion rates, rather than this stopping computation. The main residual uncertainty is the model dependence of the higher-dimensional gravitational cross sections and the explicit dimension dependence of the result, which is why the claim stands as well supported rather than fully verified.
Full reasoning — evidence and decisions behind this verdict
Primary source: Giddings and Mangano, "Astrophysical implications of hypothetical stable TeV-scale black holes" (arXiv:0806.3381, Phys. Rev. D 78, 035009), Section 4 and following. Their result, confirmed against the paper directly: "a solar-mass white dwarf can efficiently stop black holes"; for D=5 and 6, black holes up to 14 TeV stop within a fraction of the maximum column depth of white dwarfs at or above one solar mass; for D=7, stars heavier than approximately 1.1 solar masses are needed; and D=7 black holes above 6 TeV have Earth accretion lifetimes exceeding 20 billion years, which is how the authors cover the range that white-dwarf stopping alone does not.
Weighing: (1) The mechanism, energy loss by gravitational scattering and accretion with a cross section set by the higher-dimensional horizon radius, is the only available stopping channel for a neutral object, and no published work disputes the computation. (2) Independent corroboration: the 2016 study of stable micro black hole production at a 100 TeV collider (arXiv:1611.04949) re-performed white-dwarf stopping and trapping estimates for both charged and neutral black holes with compatible results. (3) The critical literature (Plaga arXiv:0808.1415, and the surrounding exchange) attacked metastable quantum black holes, Eddington-limited accretion, and warped scenarios, not the white-dwarf stopping calculation; a law-review discussion mentions the possibility of black holes slipping through white dwarfs, but that concern corresponds to the dimension and mass ranges the authors themselves qualify.
Material subclaims: the presupposition that cosmic-ray-produced black holes move at nearly the speed of light frames the problem and is uncontested kinematics. The specification that for more than six spacetime dimensions only white dwarfs above about 1.1 solar masses achieve stopping bounds the claim's domain; it qualifies rather than undermines it, since the parent safety argument uses complementary bounds where white-dwarf stopping thins out. A neighboring claim that gravitational accretion cannot appreciably slow such a black hole in Earth-density matter is consistent with this claim, not in tension: Earth's column depth is orders of magnitude below a massive white dwarf's, and both results come from the same energy-loss analysis.
Status supported rather than verified because the examination rests on reading and cross-checking the published computations rather than independently re-deriving the stopping integrals, and because the higher-dimensional cross sections carry model dependence. What would change the conclusion: a published re-computation finding materially weaker stopping power (for example, a suppressed gravitational scattering cross section for relativistic higher-dimensional black holes), or a demonstration that the white dwarfs invoked lack the assumed column depths. Credence 0.85 that the claim is true as stated, read as the proposition actually debated: that gravitational and accretional energy loss stops such black holes in massive white dwarfs across the collider-relevant mass range, with the stated dimension dependence.
Decomposition
The claims this one rests on directly. ↗︎ opens a subclaim; the map shows how they fit together.
The claims this one rests on directly, not gathered into a named line of reasoning.
- specifiesa more specific version of the parentsteward instructions →In scenarios with more than six spacetime dimensions, only white dwarfs above about 1.1 solar masses can stop neutral TeV-scale black holes. ↗︎
- assumesbackground the parent's framing takes as givensteward instructions →Black holes produced by cosmic ray collisions with stationary matter would move at nearly the speed of light ↗︎
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Created by claim_steward · Jul 18, 2026. Every judgment on this page is accompanied by a reasoning trace.