Nuclear Reaction Defines the Abyss for Black Holes express

Original: "Nuclear Constraints on $$^{12}$$C$$(α,γ)^{16}$$O and Their Impact on Black-Hole Mass Predictions"
· Akram Mukhamedzhanov
arXiv:2605.07027v1 · 2026-05-07 · CC BY 4.0 · 1 min
Refined nuclear reaction marks the edge of the abyss: ordinary black holes weigh between 61 and 75 Suns.

Gravitational waves have laid bare an abyss: black holes with masses between 60 and 120 Suns are almost never born. This chasm is carved out by pair-instability supernovae — explosions that leave not even a speck of the star. Whether the star falls into the abyss or survives on its edge depends on the reaction of carbon with helium, which governs the core composition.

This process is leisurely: even a tiny speedup would turn all carbon into oxygen, depriving the universe of life. Fred Hoyle first realized the reaction is tuned exquisitely finely, otherwise carbon would be hundreds of times scarcer. New data have narrowed the possible rates by nearly half. It turns out the edge of the abyss lies farther out than thought: the lightest ordinary black holes start at 61–75 solar masses. A shift of just a couple percent, and the boundary leaps by tens of masses.

The carbon-helium reaction is so slow that the slightest acceleration would deprive the universe of carbon-based life.

\frac{M_{\rm BH}}{M_\odot}\simeq 61\text{--}75
lower mass limit for pair-instability black holes in solar masses
Scientists
Fred HoyleSubrahmanyan ChandrasekharFritz ZwickyJacob BekensteinKarl SchwarzschildRalph Alpher
Concepts
nuclear reaction mass gap black hole mass gap First law of black hole mechanics Chandrasekhar limit critical collapse logarithmic correction no-hair theorem hawking area law Hawking area theorem accretion rate quantum corrections gw190814 core collapse event horizon stability innermost stable circular orbit ringdown quasar feedback barrow entropy wald entropy mass–energy equivalence