The Influence of the ^8B(α,p)^11CReaction in Supermassive Stars

Details The Influence of the ^8B(α,p)^11CReaction in Supermassive Stars The Influence of the ^8B(α,p)^11CReaction in Supermassive Stars

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..dnp.gf002r&link_type=abstract

American Physical Society, Division of Nuclear Physics Fall Meeting, October 30 - November 1, 2003, Tucson, Arizona, MEETING ID:

Physics

Nuclear Physics

Scientific paper

The ^8B(α,p)^11C reaction is part of the network that can bypass the triple α process leading to the production of ^12C. We have measured the astrophysical reaction rate for this reaction by studying the inverse ^11C(p,α)^8B process. The radioactive ^11C beam was produced via the p(^11B,^11C)n reaction using the in-flight facility installed at the ATLAS accelerator. The outgoing particles (^8B and α) were detected in coincidence in an annular ionization chamber silicon-strip detector system with a detection efficiency of about 60%. Information about transitions to excited states populated in the ^8B(α,p)^11C reaction were obtained through a simultaneous measurement of inelastic scattering ^11C(p,p')^11C. The astrophysical reaction rate obtained from the excitation function measured in the energy range E_x=8.8-10 MeV was found to be a factor of 10-50 higher than previous estimates. The influence of these higher rates on various astrophysical sites will be discussed. This work was supported by the US Department of Energy, Nuclear Physics Division, under contract No. W-31-109-ENG-38 and by a NATO Collaborative Linkage Grant.

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