Speaker
Description
Among the reactions driving stellar evolution, $^{12}$C + $^{12}$C fusion gives the key ingredients during carbon burning. This system reveals many resonances [1], but also regions with suppressed fusion cross-sections [2,3]. The reaction was recently measured by the STELLA collaboration utilizing the gamma-particle coincidence technique for precise cross-section measurements reaching down to the Gamow window of massive stars. From the experimental data, reaction rates were determined by approximating a hindrance trend and by adding on top a resonance at the lowest measured energy. The impact of these reaction rates on the evolution of massive stars was explored with models of 12 and 25M$_{\odot}$ using the stellar evolution code GENEC [4], and a detailed study of the resulting nucleosynthesis with a 1454 elements network [5] was performed. The sensitivity of the STELLA experimental cross-sections on the temperature range for C-burning for the stellar models studied will be presented. The final abundances and their impacts on stellar evolution will be discussed in detail in this contribution [6].
[1] Aguilera, E. F., Rosales, P., Martinez-Quiroz, E., et al. 2006, Phys. Rev. C, 73, 064601
[2] Fruet, G., Courtin, S., Heine, M., et al. 2020, Phys. Rev. Lett., 124, 192701
[3] Tan, W. P., Boeltzig, A., Dulal, C., et al. 2020, Phys. Rev. Lett., 124, 192702
[4] Eggenberger, P., Meynet, G., Maeder, A., et al. 2008, Astrophys. Space Sci., 316, 43
[5] Choplin, A., Maeder, A., Meynet, G., & Chiappini, C. 2016, A&A, 593, A36
[6] Monpribat, E., Martinet, S., Courtin, S., et al. 2022, A&A, 660, A47
