Other
Scientific paper
Jan 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phdt........15z&link_type=abstract
Thesis (PH.D.)--YALE UNIVERSITY, 1993.Source: Dissertation Abstracts International, Volume: 54-06, Section: B, page: 3127.
Other
6
Scientific paper
Helium burning plays a key role in both the formation of heavy elements and the collapse of massive stars. The result of the helium burning--the ^{12 }C/16O ratio, determines the abundance of heavy elements and the dynamics of a massive star at its final stages before a supernova explosion. One of the two reactions in the helium burning process, the 12C( alpha,gamma)16O capture reaction, is poorly understood despite intense theoretical and experimental work during the last two decades. The previously extracted p-wave 'S-factor' for the 12C(alpha,gamma) 16O capture reaction at 300 keV (SE1(300)) ranges in value from 0 to 500 keV-barn. On the other hand, the beta-delayed alpha-particle emission spectrum at low energy provides a very sensitive means to determine the reduced alpha-particle width of the bound 1^- state, hence the 'S-factor'. The spectrum of low energy beta-delayed alpha -particle emission 16N, was measured with high sensitivity; e.g., at E _spα{L} ~ 1 MeV a sensitivity for a beta-decay branching ratio in the range of 10^{-9} (to 10^{-10}) was achieved. The branching ratio and spectrum of beta -decay of 16N to the relevant broad 1^- resonance were remeasured. The alpha-particle spectra were unfolded to remove effects of finite energy resolution (foil thickness). We used previous theoretical work of Ji, Filippone, Humblet and Koonin to extract from these data the astrophysical E1 S-factor for the 12C( alpha,gamma)16O capture reaction and find SE1(300) = 95 +/- 6 (stat) +/- 28 (syst) keV-barn.
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