On the properties of electromagnetically separated noble gas targets for nuclear reaction studies

Strengths of the resonances at 436, 479, 639, 661, and 1279 keV in theNe22(p,γ)Na23Depalo1, Cavanna2, Ferraro3 et al. 2015Phys. Rev. C425585View full textAdd to dashboardCite

“…Therefore, 22 Ne can still be present in second generation stars or whenever material processed by the CNO cycle is mixed with helium-rich material [4]. The neutrons stored in 22 Ne have recently been suggested to play a role in neutron capture nucleosynthesis in supernova of type Ia that may lay the seed for an alternative production of p-nuclei [5][6][7].…”

“…At temperatures T > 70 MK, proton capture surpasses the decay, and 22 Ne is effectively bypassed in the NeNa cycle. In this scenario, the destruction of 22 Ne by the 22 Ne(p,γ) 23 Na reaction is no longer compensated by fresh production.…”

“…18 F(β + ν) 18 O(α,γ) 22 Ne. Therefore, 22 Ne can still be present in second generation stars or whenever material processed by the CNO cycle is mixed with helium-rich material [4].…”

“…Whithin the cycle, 22 Ne can only be produced by the decay of radioactive 22 Na (T 1/2 = 2.6027 y [2]). However, this decay competes with proton capture on 22 Na [3]. At temperatures T > 70 MK, proton capture surpasses the decay, and 22 Ne is effectively bypassed in the NeNa cycle.…”

“…However, in a helium burning scenario 22 Ne may be produced from the ashes of the carbonnitrogen-oxygen (CNO) cycle, using the chain: 14 N(α,γ)…”