^18F(a,p)^21Ne reaction study for astrophysical implications

Details ^18F(a,p)^21Ne reaction study for astrophysical implications ^18F(a,p)^21Ne reaction study for astrophysical implications

Oct 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aps..dnp.ce012l&link_type=abstract

American Physical Society, Division of Nuclear Physics Annual Meeting, October 25-28, 2006, abstract #CE.012

Physics

Nuclear Physics

Scientific paper

As an alternative neutron source for the weak r-process, one of models suggested the r-process nucleosynthesis in the supernova shock passing through the He-rich shell of the pre-supernova star. In this helium rich environment, a possible neutron source for the second r-process would be the reaction sequence ^14N(α,γ)^18F(α,p)^21Ne(α,n)^24Mg with rapid depletion of ^14N. The (α,p) reaction on ^18F will be faster than β^+ decay at the high densities and temperature in the shock. The ^18F(α,p)^21Ne reaction and the inverse reaction ^21Ne(p,α)^18F have been measured in the energy range of the Gamow window. Experimental results will be presented and compared with Hauser-Feshbach calculations and the interests in nuclear physics. The astrophysical implications of the new reaction rates will be discussed.

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