Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios

Details Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios

Mar 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1098..181p&link_type=abstract

FUSION08: New Aspects of Heavy Ion Collisions Near the Coulomb Barrier. AIP Conference Proceedings, Volume 1098, pp. 181-186 (2

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Nuclear Structure Models And Methods, Gas-Filled Counters: Ionization Chambers, Proportional, And Avalanche Counters, Calorimeters, Nucleosynthesis In Novae, Supernovae, And Other Explosive Environments, Radiation Detectors

Scientific paper

In astrophysics, the first excited 0+ state of 12C at 7.654 MeV (Hoyle state) is the most important in the triple-α process for carbon nucleosynthesis. In explosive scenarios like supernovae, where temperatures of several 109 K are achieved, the interference of the Hoyle state with the second 0+ state located at 10.3 MeV in 12C becomes significant. The recent NACRE compilation of astrophysical reaction rates assumes a 2+ resonance at 9.1 MeV for which no experimental evidence exists. Thus, it is critical to explore in more detail the 7-10 MeV excitation energy region, especially the minimum between the two 0+ resonances for carbon nucleosynthesis. The states in 12C were populated through the β-decay of 12B and 12N produced at the ATLAS (Argonne Tandem Linac Accelerator System) in-flight facility. The decay of 12C into three alphas is detected in a Frisch grid twin ionization chamber, acting as a low-threshold calorimeter. This minimizes the effects of β-summing and allowed us to investigate the minimum above the Hoyle state with much higher accuracy than previously possible. A detailed data analysis will include an R-matrix fit to determine an upper limit on the 2+ resonance width.

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