The Study of the Deuteron + LITHIUM-8 Reaction at Astrophysical Energies

Details The Study of the Deuteron + LITHIUM-8 Reaction at Astrophysical Energies The Study of the Deuteron + LITHIUM-8 Reaction at Astrophysical Energies

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996phdt.........6l&link_type=abstract

Thesis (PH.D.)--UNIVERSITY OF NOTRE DAME, 1996.Source: Dissertation Abstracts International, Volume: 57-03, Section: B, page: 18

Astronomy and Astrophysics

Astrophysics

Beryllium

Scientific paper

The astrophysically relevant d(^8 Li,^9Be^*) n reaction cross section was measured at the ^8Li incident energies of 13.8 MeV, 10.7 MeV, 7.4 MeV, and 6.0 MeV. The excited states in ^9Be^* are particle unstable and decay by neutron emission, therefore this reaction destroys ^9Be in the Inhomogeneous Big Bang model. The resulting ^8Be nucleus is also unstable, decaying from the ground state into two ^4He nuclei. In this experiment, it is these two ^4He nuclei that were detected in coincidence using a double-sided silicon strip detector to measure the energies of the ^4He nuclei. Then by reconstruction, the angular distributions for the ^8Be nucleus can be obtained. Due to the missing energy from the neutrons, it was not possible to experimentally reconstruct the ^9Be^* angular distribution. A Monte Carlo calculation was used to determine the total reaction cross section. We investigate the role that different assumptions have on the value of the total reaction cross section by monitoring the yield of the ^8Be nucleus: from isotropic production versus a Distorted Wave Born Approximation production and from selecting different states for the decay ^9Be ^*. Angular distributions are presented for the ^8Be after reconstruction for each energy under these assumptions. Energy spectrums for the ^4He nuclei are also presented. The total reaction cross sections are presented for all of the assumptions, as well as the S-factor for astrophysical interest. The d+ ^8Li reaction to excited states in ^9Be was determined to be 29.6+/-9.4 mb cross section. This indicates a reduction in abundance for ^9Be, which will have to incorporated into theoretical models for the origin of the elements.

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