| Issue |
EPJ Web Conf.
Volume 165, 2017
Nuclear Physics in Astrophysics VIII (NPA8 2017)
|
|
|---|---|---|
| Article Number | 01007 | |
| Number of page(s) | 4 | |
| DOI | https://doi.org/10.1051/epjconf/201716501007 | |
| Published online | 30 December 2017 | |
https://doi.org/10.1051/epjconf/201716501007
The astrophysical S-factor of the direct 18O(p, γ)19F capture by the ANC method
1 Nuclear Physics Institute of Czech Academy of Sciences, 250 68 Řež, Czech Republic
2 Cyclotron Institute, Texas A&M University, College Station, TX 77843
3 Università di Catania and INFN Laboratori Nazionali del Sud, Catania, Italy
* e-mail: burjan@ujf.cas.cz
Published online: 30 December 2017
We attempted to determine the astrophysical S-factor of the direct part of the 18O(p, γ)19F capture by the indirect method of asymptotic normalization coefficients (ANC). We measured the differential cross section of the transfer reaction 18O(3He, d)19F at a 3He energy of 24.6 MeV. The measurement was realized on the cyclotron of the NPI in Řež, Czech Republic, with the gas target consisting of the high purity 18O (99.9 %). The reaction products were measured by eight ∆E-E telescopes composed from thin and thick silicon surface-barrier detectors. The parameters of the optical model for the input channel were deduced by means of the code ECIS and the analysis of transfer reactions to 12 levels of the 19F nucleus up to 8.014 MeV was made by the code FRESCO. The deduced ANCs were then used to specify the direct contribution to the 18O(p, γ)19F capture process and were compared with the mutually different results of two works.
© The Authors, published by EDP Sciences, 2017
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (http://creativecommons.org/licenses/by/4.0/).
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