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Accretion of Primordial Black Holes in Stellar Interiors

  • Authors: Matteo Cantiello, Ore Gottlieb, Cameron Norton, Matthew Kleban, Ken Van Tilburg

Matteo Cantiello et al 2026 The Astrophysical Journal 1010 .

  • Provider: AAS Journals

Caption: Figure B2.

Effective Knudsen number at the circularization radius (computed from Equation (B4)) as a function of specific angular momentum, for MBH = 10−16 M⊙. The hatched bands mark the excluded loss-cone (ℓ < ℓcrit) and reflected (﹩\ell \gt {\ell }_{{\rm{\max }}}﹩) populations. The pileup enhancement ξ(ℓ) is sufficient to make Kneff < 1 for the bulk of the recycling population (ℓ ≳ ℓ⋆ ≃ 12ℓcrit), so most circularization radii are self-collisionalized. Only a low-ℓ tail (∼21%) remains in the formally collisionless “reservoir” regime; the additional mass needed to push these bins to Kneff ∼ 1 is ∼6 × 10−15 g and accumulates in only a few freefall times.

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