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The 19F(α, p)22Ne Reaction at Energies of Astrophysical Relevance by Means of the Trojan Horse Method and Its Implications in AGB Stars

  • Authors: G. D'Agata, R. G. Pizzone, M. La Cognata, I. Indelicato, C. Spitaleri, S. Palmerini, O. Trippella, D. Vescovi, S. Blagus, S. Cherubini, P. Figuera, L. Grassi, G. L. Guardo, M. Gulino, S. Hayakawa, R. Kshetri, L. Lamia, M. Lattuada, T. Mijatovic`, M. Milin, Đ. Miljanic`, L. Prepolec, G. G. Rapisarda, S. Romano, M. L. Sergi, N. Skukan, N. Soic`, V. Tokic`, A. Tumino, and M. Uroic`

2018 The Astrophysical Journal 860 61.

  • Provider: AAS Journals

Caption: Figure 9.

Experimental angular distribution for the 19F(α, p)22Ne reaction (﹩\tfrac{d\sigma }{d{\rm{\Omega }}}﹩ vs. ϑC.M, where ϑC.M is the emission angle of the proton in the center-of-mass reference frame of the reaction). The blue solid circles are the present experimental data. The red line represents a fit to the experimental data done by means of a linear combination of Jπ = 3/2+ and Jπ = 5/2+ angular distributions, using the equations given in Blatt & Biedenharn (1952) and La Cognata et al. (2015). The black, green, and blue lines are instead angular distributions for Jπ equal to 3/2(with ﹩{{\rm{a}}}_{3/{2}^{-}}﹩ as normalization coefficient), 1/2+, and 1/2 (multiplied by a factor of two to separate it from the preceding distribution). See the text for details.

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