The SE1 factor of the 12C(α,γ)16O Reaction and the 16N β-delayed α Decay

Details The SE1 factor of the 12C(α,γ)16O Reaction and the 16N β-delayed α Decay The SE1 factor of the 12C(α,γ)16O Reaction and the 16N β-delayed α Decay

Jan 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc..972..261t&link_type=abstract

EXOTIC NUCLEI AND NUCLEAR/PARTICLE ASTROPHYSICS (II): Proceedings of the Carpathian Summer School of Physics 2007. AIP Conferen

Astronomy and Astrophysics

Astrophysics

1

Nuclear Explosions, Nuclear Reaction Models And Methods, Resonance Reactions, Alpha Decay

Scientific paper

The 12C(α,γ)16O reaction is of great importance for the understanding the nuclear synthesis and explosion mechanism of the supernova. The cross section at the relevant stellar burning energies, around 300 keV, is dominated by the sub-threshold resonances. The 16N β-delayed α decay data provide the most sensitive constrain on this sub-threshold resonance. Using twin-ionization chambers, we have measured the α particles and 12C recoil nuclei in coincidence. The spectrum has been fitted together with the published 12C(α,γ)16O data and the elastic scattering phase shift data using R-matrix. The SE1 factor at 300 keV has been determined as 73+/-21 keVb.

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