EPJ Web Conf.
Volume 136, 2017RICAP16, 6th Roma International Conference on Astroparticle Physics
|Number of page(s)||4|
|Section||Particle and Astroparticle|
|Published online||23 March 2017|
Feasibility study of the 13C(α, n)16O reaction at LUNA
1 INFN, Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi, Italy
2 Gran Sasso Science Institute, INFN, Viale F. Crispi 7, 67100, L’Aquila, Italy
a e-mail: email@example.com
Published online: 23 March 2017
The 13C(α, n)16O reaction determines the dominant neutron source of the sprocess in thermally pulsing, low-mass, asymptotic giant branch (TP-AGB) stars. The temperature during the s-process in the 13C pocket of 90×106 K corresponds to a Gamow window of 140-230 keV. Since this energy is far below the Coulomb barrier, the cross section of this reaction is extremely small and its rate can only be extrapolated from the measurements at higher energies. At present, the cross section at Gamow peak is uncertain by almost one order of magnitude.
An experimental campaign aimed at measuring low energy cross section in 13C(α n)16O is scheduled at the underground LUNA-400 accelerator in Gran Sasso Laboratory, Italy. The unique underground location of this facility offers significant improvement in sensitivity compared with previous investigations. It will allow to establish the interference pattern of the resonances and the absolute scale of this reaction.
© 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.
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