Abstract
The carbon fusion reaction is crucial in stellar evolution. Despite six decades of studies, there is still a large uncertainty in the reaction rate which limits our understanding of various stellar objects, such as massive stars, type Ia supernovae, and superbursts. In this paper, we review the experimental and theoretical studies of the carbon fusion reaction at sub-barrier energies. An outlook for future studies is also presented.
Highlights
Stars with a mass of more than 8 solar masses and less than 10 solar masses can ignite the 12C+12C fusion reaction and proceed with carbon burning inside of their cores
More massive stars will continue with Ne, Oand Si-burnings in their cores and shells and eventually become supernovae
In type Ia supernova, the ignition happens in the core of white dwarf typically at T∼ 0.15-0.7 GK
Summary
Stars with a mass of more than 8 solar masses and less than 10 solar masses can ignite the 12C+12C fusion reaction and proceed with carbon burning inside of their cores. These stars end up their lives as Ne/O white dwarfs. More massive stars will continue with Ne-, Oand Si-burnings in their cores and shells and eventually become supernovae. During these hydrostatic and explosive burning processes, 12C+12C is one of the primary reactions of the burning processes which shape the stellar evolution and the final nucleosynthesis. In type Ia supernova, the ignition happens in the core of white dwarf typically at T∼ 0.15-0.7 GK. The ignition conditions mentioned above strongly depend on the 12C+12C reaction rate as well as the treatment of reaction rate estimation in dense matter[4,5,6]
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