Fraile Prieto, Luis Mario2023-06-182023-06-1820161742-658810.1088/1742-6596/665/1/012031https://hdl.handle.net/20.500.14352/24368© Iop Publishing Ltd. Articulo firmado por más de 10 autores. Nuclear Physics in Astrophysics Conference (NPA) (6 .2013. Lisboa, Portugal). This work was supported by the Spanish Ministerio de Economía y Competitividad under Grants CONSOLIDER-Ingenio 2010 CSD2008-0037 (CUP), PRI-PIMNUP-2011-1348, FPA2011-28770-C03-03, FPA2011-24553, FPA2010-17142 and CSD-2007-00042 (CPAN).The reactions C-13(alpha,n)O-16 and Ne-22(alpha,n)Mg-25 are the primary sources of neutrons for the astrophysical s-process. The feasibility of cross section measurements within the respective Gamow windows is discussed in quantitative terms for a 4 pi neutron counter, based on He-3 tubes and a neutron moderator, placed in an underground lab.engAtribución 3.0 Españahttps://creativecommons.org/licenses/by/3.0/es/journal articlehttp://dx.doi.org/10.1088/1742-6596/665/1/012031http://iopscience.iop.org/open access539.1Astronomy & AstrophysicsPhysicsNuclearFísica nuclear2207 Física Atómica y Nuclear