Constraining the 12C+12C fusion cross section for astrophysics

• Main Authors: Bucher, B, Fang, X, Tang, X D, Tan, W P, Almaraz-Calderon, S, Alongi, A, Ayangeakaa, AD, Beard, M, Best, A, Browne, J, Cahillane, C, Couder, M, Dahlstrom, E, Davies, P, deBoer, R, Kontos, A, Lamm, L, Long, A, W Lu, Lyons, S, C Ma, Moncion, A, Notani, M, Patel, D, Paul, N, Pignatari, M, Roberts, A, Robertson, D, Smith, K, Stech, E, Talwar, R, Thomas, S, Wiescher, M
• Format: Conference Proceeding
• Language: English
• Subjects: Astronomical models; Astrophysics; Carbon 13; Constraint modelling; Cross-sections; Energy measurement; Massive stars; Nuclear reactions; Stellar evolution; Supernovae
• ISSN: 2101-6275; 2100-014X
• DOI: 10.1051/epjconf/20159303009

The 12C+12C reaction is one of the single most important nuclear reactions in astrophysics. It strongly influences late evolution of massive stars as well as the dynamics of type Ia supernovae and x-ray superbursts. An accurate estimation of the cross section at relevant astrophysical energies is extremely important for modeling these systems. However, the situation is complicated by the unpredictable resonance structure observed at higher energies. Two recent studies at Notre Dame have produced results which help reduce the uncertainty associated with this reaction. The first uses correlations with the isotope fusion systems, 12C+13C and 13C+13C, to establish an upper limit on the resonance strengths in 12C+12C. The other focuses on the specific channel 12C+12C→23Mg+n and its low-energy measurement and extrapolation which is relevant to s-process nucleosynthesis. The results from each provide important constraints for astrophysical models.