Abstract
Carbon burning is a key step in the evolution of massive stars, Type 1a supernovae and superbursts in x-ray binary systems. Determining the fusion cross section at relevant energies by extrapolation of direct measurements is challenging due to resonances at and below the Coulomb barrier. A study of the reaction has identified several states in , close to the threshold, which predominantly decay to . These states were not observed in resonance scattering suggesting that they may have a dominant cluster structure. Given the very low angular momentum associated with sub-barrier fusion, these states may play a decisive role in fusion in analogy to the Hoyle state in helium burning. We present estimates of updated fusion reaction rates.
- Received 9 May 2021
- Revised 23 July 2021
- Accepted 26 July 2022
DOI:https://doi.org/10.1103/PhysRevLett.129.102701
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