HIGHLIGHTS
SUMMARY
Carbon burning is one of the main advanced stages in the evolution of massive stars (M > 8·M⊙ ) and type Ia supernovae. In the aforementioned astrophysical scenarios, the 12 C +16 O fusion proceeds through the following reaction_channels: 12 C(16 O, α)24 Mg (Q=6.77 MeV), 12 C(16 O, p)27 Al (Q=5.17 MeV) and partially 12 C(16 O, n)27 Si (Q=- 0.424 MeV). The second-stage detectors were calibrated both in energy and position with devoted experimental runs using an eight-peak alpha source, elastic . . .
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