Author:
Petruse T,Guardo G. L.,Cognata M. La,Lattuada D.,Spitalieri C.,Balabanski D. L.,Agiksoz E.,Acosta L.,Capponi L.,Carbone D.,Cherubini S.,Choudhury D.,D’Agata G.,Pietro A. Di,Figuera P.,Gulino M.,Kilik A. I.,Commara M. La,Lamia L.,Matei C.,Palmerini S.,Pizzone R. G.,Romano S.,Soderstrom P.-A.,Sparta R.,Tumino A.,Onses S. Vinales
Abstract
The 19F(ρ,α)16O reaction is an important fluorine destruction chan- nel in the proton-rich outer layers of asymptotic giant branch (AGB) stars and it might also play a role in hydrogen-deficient post-AGB star nucleosynthesis. At present, theoretical models overproduce F abundances in AGB stars with re-spect to the observed values, thus calling for further investigation of the nuclear reaction rates involved in the production and destruction of fluorine. In the last years, new direct and indirect measurements improved significantly the knowl- edge of 19F(ρ,α)16O cross section at deeply sub-Coulomb energies (below 0.8 MeV). However, those data are larger by a factor of 1.4 with respect the previ- ous data reported in the NACRE compilation in the energy region 0.6-0.8 MeV. Using the Large High resolution Array of Silicons for Astrophysics (LHASA), we performed a new direct measurement of the 19F(ρ,α)16O. The goal of this experiment is to reduce the uncertainties in the nuclear reaction rate of the 19F(ρ,α)16O reaction. Here, experimental details, the calibration procedure and angular distributions are presented.
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