The E2 Contribution to the ^12 C(α ,γ )^16O Reaction

Details The E2 Contribution to the ^12 C(α ,γ )^16O Reaction The E2 Contribution to the ^12 C(α ,γ )^16O Reaction

Apr 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aps..apr..j104t&link_type=abstract

American Physical Society, APS/AAPT Joint Meeting, April 18-21, 1997, abstract #J1.04

Astronomy and Astrophysics

Astrophysics

Scientific paper

Accurate knowledge of the astrophysical reaction rate for the ^12 C(α ,γ )^16O reaction is a long standing problem. The desired accuracy for the total rate is 10%. In recent years progress has been made to determine the rate for the E1- part with an accuracy of about 15% for energies relevant for astrophysics. This progress has been achieved by Buchmann et al. through a simultaneous fit of three types of data: the ^12C(α ,γ)^16O, the ^12C(α ,α )^12C and the β -delayed α -particle decay data from ^16N. However, in a subsequent paper, the same authors came to the conclusion that for the E2- part only an upper limit of 140 keV b can be given for S_E2(300), based on analysis of available ^12C(α ,γ)^16O and elastic scattering data. We have investigated the quality of the input data to above analysis which will be discussed along with the results of a newly performed E2 measurement. In this experiment the sum of E1 and E2 was measured with a large BGO-detector in close geometry whereas the E1 part was obtained simultaneously with a small detector in far geometry, thus observing the E1-radiation nearly free of the E2 contribution for the first time. These data will be presented. In addition, an attempt was made to measure the energy dependence of the cross section near the narrow J^π =2^+-resonance to determine the sign of the interference between the background and this resonance with a thin gas target and a large 4π - NaI detector. Good knowledge of this interference structure can yield an absolute determination of the nonresonant E2 contribution at this energy. Preliminary results will be shown.

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