Schematic overview of the three spherical-accretion regimes and the disk-accretion regime onto a PBH embedded in a stellar interior, ordered by increasing M_BH. Hot Bondi (M_BH ≲ 10⁻¹⁴ M_⊙): the Bondi sphere is optically thin (τ < 1); bremsstrahlung photons (orange wavy arrows) escape freely without interacting with the infalling gas (gray arrows), yielding η ≈ 0.01–0.1, peaking near 10⁻¹⁵ M_⊙. Bremsstrahlung cooling (10⁻¹⁴–5 × 10⁻¹³ M_⊙): bremsstrahlung cooling (green region) drains thermal energy before the gas reaches pair-producing temperatures; the flow approaches isothermal (T → T_∞) and η ≈ 10⁻². Photon trapping (5 × 10⁻¹³ ≲ M_BH/M_⊙ ≲ 10⁻²): the Bondi sphere is optically thick; in spherical geometry the trapping radius r_trap moves outward from r_S and most locally produced photons are advected inward rather than escaping (M. C. Begelman 1979). The escaping luminosity is bounded by ∼0.6L_Edd but does not cap the accretion rate, and ﹩\dot{M}\approx {\dot{M}}_{{\rm{B}}}﹩ throughout. Disk accretion (M_BH ≳ 10⁻² M_⊙, depending on stellar rotation): once r_circ > r_ISCO a thin disk forms, η ≈ 0.08, and the standard Eddington limit applies via viscous angular-momentum transport (O. Gottlieb et al. 2026).