Determination of the stellar reaction rates of ^17O(α,n)^20Ne and ^17O(,)^21Ne

Details Determination of the stellar reaction rates of ^17O(α,n)^20Ne and ^17O(,)^21Ne Determination of the stellar reaction rates of ^17O(α,n)^20Ne and ^17O(,)^21Ne

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aps..dnp.cg004b&link_type=abstract

American Physical Society, 2010 Fall Meeting of the APS Division of Nuclear Physics, November 2-6, 2010, abstract #CG.004

Physics

Nuclear Physics

Scientific paper

The reaction ^16O(n, γ)^17O acts a neutron poison in the weak s-process by reducing the number of available neutrons in the stellar burning environment. The captured neutrons can be re-emitted into the stellar environment via the reaction ^17O(n, n)^20Ne, weakening the poisoning effect of ^16O. This channel competes with the reaction ^17O(,)^21Ne, so that in order to determine the strength of ^16O as a neutron poison it is important to know the reaction of both channels. Only limited information is available on the ^16O(,)^20Ne and especially on the ^16O(,)^21Ne reaction, which leads to large uncertainties in the determination of the abundance production of the weak s-process. The (,) channel has been measured in the energy range from 900 keV to 2300 keV using a high efficiency 4π neutron detector. To improve the efficiency determination of the detector the (,1) channel has been measured separately via gamma-ray spectroscopy and the detector response to the resulting neutron energy distribution has been modeled in a Geant4 simulation. An initial measurement of the (,) channel has been successfully completed and a second experiment using the new 5 HPGe detector array GEORGINA is in planning. Results of the finished experiments and the planned experiment will be discussed.

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