premise-b-compact-star-accretion

Orientation — Premise B (stable-BH-still-harmless) + compact-star accretion physics

Slice: the astrophysical-survival argument that even a stable micro black hole would be harmless, and the accretion physics + compact-star observations it depends on.

Sources by topic

The load-bearing pair (Giddings-Mangano):

• S-37 - Giddings & Mangano 2008 — Astrophysical implications of hypothetical stable TeV-scale black holes — the paper Premise B is built on: subatomic capture → Bondi accretion → Eddington feedback timescales, plus the WD/NS survival bound.
• S-42 - Giddings & Mangano 2008 — Comments on claimed risk from metastable black holes (reply to Plaga) — their formal reply defending the argument against Plaga’s metastable-BH loophole.

Independent/parallel derivation:

• S-47 - Koch, Bleicher & Stöcker 2009 — Exclusion of black hole disaster scenarios at the LHC — a second derivation reaching the same conclusion; useful to check whether “no risk” is robust across authors or is one argument echoed.

Accretion physics underlying the growth-timescale calculation:

• S-51 - Bondi 1952 — On spherically symmetrical accretion — the classical macroscopic accretion-rate formula G-M apply once a stable BH is large enough for gravitational (not quantum) capture.
• S-57 - Unruh 1976 — Absorption cross section of small black holes — the quantum absorption-cross-section physics governing the earliest, sub-macroscopic growth phase, before Bondi accretion applies.

Independent compact-star empirical inputs (the “would-have-already-destroyed-them” bound):

• S-66 - Demorest et al. 2010 — Shapiro delay measurement of a two-solar-mass neutron star — precision mass measurement establishing real neutron stars reach ~2 M_sun / nuclear density and are old binary-pulsar systems.
• S-61 - Kepler et al. 2007 — White dwarf mass distribution in the SDSS — large-sample SDSS mass catalog establishing the white-dwarf population’s mass/density distribution (up to ~1.33 M_sun).
• S-70 - Hansen et al. 2007 — Cooling of white dwarfs and the age of the globular cluster NGC 6397 — direct cooling-age evidence that white dwarfs survive undisturbed for >11 Gyr.

search_scope

Targeted search (not a broad literature survey, per brief’s narrow scope): direct lookup of the two named load-bearing papers (arXiv 0806.3381 and its Plaga reply, found by searching “Giddings Mangano reply Plaga” which surfaced 0808.4087) and the named Koch-Bleicher-Stöcker paper; WebFetch of the arXiv abstract/ar5iv HTML of 0806.3381 to extract its own reference list for the accretion-physics primaries it leans on (Bondi/Bondi-Hoyle-Lyttleton for macroscopic accretion; the paper’s subatomic-capture discussion led to Unruh 1976 for the underlying absorption-cross-section physics). For the compact-star observational leg, targeted keyword searches for one representative primary each on white-dwarf masses (SDSS catalog → Kepler et al. 2007), neutron-star mass (precision pulsar timing → Demorest et al. 2010, chosen for its landmark 2 M_sun Shapiro-delay result), and white-dwarf cooling age (globular-cluster WD sequence → Hansen et al. 2007, NGC 6397). Did not exhaustively mine stellar astrophysics per brief’s instruction.

exclusions

• Rainer Plaga’s own critique (arXiv:0808.1415, “On the potential catastrophic risk from metastable quantum-black holes”) — surfaced repeatedly while researching the reply, but explicitly assigned to slice 6; not minted here, only referenced via found_via on S-42.
• Bondi & Hoyle 1944 / Hoyle & Lyttleton 1939 (earlier stages of the Bondi-Hoyle-Lyttleton accretion formula) — not separately minted; treated as superseded/consolidated by the standard single citable Bondi 1952 MNRAS paper, which is the version most directly tied to the formula Giddings-Mangano actually apply.
• Lattimer & Prakash 2001/2021 neutron-star equation-of-state reviews — found while searching for NS density data, but these are synthesis/review articles, not primary observational measurements; excluded per the primary-source rule (mined only as background, no node).
• Christensen & Fulling (trace-anomaly Hawking-radiation derivation), Schwinger 1951 (pair production), Gregory-Laflamme, higher-dimensional Kerr — all appear in Giddings-Mangano’s reference list but belong to slice 2’s territory (evaporation theory, BH production/higher-dim gravity) or are used only incidentally; not minted here.
• Various neutron-star cooling/thermal-age papers (isolated NS cooling, spin-down ages) surfaced during search but not minted — Demorest 2010 + Hansen 2007 already give one age-bearing data point each for NS and WD respectively, per the brief’s “a FEW representative” instruction; did not add a second NS-age paper to avoid over-mining a narrow slice.

Shape of the slice

Small and tight by design (8 sources vs. a nominal 20-note budget): the brief explicitly scoped this to “own the load-bearing paper + its reply + accretion physics + a few representative compact-star primaries, do not exhaustively mine stellar astrophysics.” The two Giddings-Mangano papers plus Koch-Bleicher-Stöcker form the argument’s spine; Bondi 1952 and Unruh 1976 are the two classical-physics inputs the growth-timescale calculation is built from; Demorest 2010, Kepler 2007, and Hansen 2007 are one representative primary each for neutron-star mass/density, white-dwarf mass/density, and white-dwarf survival-age respectively — enough to make the “independent compact-star dataset” concrete without turning this into a stellar-astrophysics literature review. I could not confirm citation counts for any source within the search budget (WebSearch did not surface Semantic Scholar/INSPIRE citation figures directly); all citation_count fields are left unknown for step 2 to fill in if needed. I did not find a distinct primary paper for the electromagnetic/Coulomb-capture phase of subatomic accretion — Giddings-Mangano’s own text states this calculation is their own, with no specific prior citation, so no separate node exists for it.