Astrophysically Important 26Si States Studied with the 28Si(4He,6He)26Si Reaction

Classical-Nova Contribution to the Milky Way’sAl26Abundance: Exit Channel of the KeyAl25(pBennett1, Wrede2, Chipps3 et al. 2013Phys. Rev. Lett.Self Cite477732View full textAdd to dashboardCite

“…Direct measurements of the resonance strengths using a 25 Al ( ¼ 10:4 s) beam are not yet possible at rare-isotope beam facilities due to insufficient intensities. Efforts to constrain the reaction rate indirectly by studying the proton-unbound states and mass of 26 Si have included a variety of experimental nuclear-physics methods utilizing both stable and rare isotope beams [20,21,[24][25][26][27][28][29][30][31][32][33][34][35]. In addition, reaction-rate evaluations employing available data and supplemented by shellmodel calculations or information from the isospin mirror nucleus 26 Mg have been conducted [16,23,[36][37][38].…”

Classical-Nova Contribution to the Milky Way's $^{26}$Al Abundance: Exit Channel of the Key $^{25}$Al($p,γ$)$^{26}$Si Resonance

“…Direct measurements of the resonance strengths using a 25 Al (τ = 10.4 s) beam are not yet possible at rare-isotope beam facilities due to insufficient intensities. Efforts to constrain the reaction rate indirectly by studying the proton-unbound states and mass of 26 Si have included a variety of experimental nuclearphysics methods utilizing both stable and rare isotope beams [20,21,[24][25][26][27][28][29][30][31][32][33][34][35]. In addition, reaction-rate evaluations employing available data and supplemented by shell-model calculations or information from the isospin mirror nucleus 26 Mg have been conducted [16,23,[36][37][38].…”

Beta decay of 26 P to determine the 25 Al(p, γ) 26 Si reaction rate in novae

“…These uncertainties were as large as an order of magnitude in 2006 and resulted in a factor of 3.4 variation in the amount of 26 Al expected to be produced by a nova on a 1.35 solar mass ONeMg white dwarf. The large uncertainty in the reaction rate was due to the uncertainty in the 25 Al(p, γ) 26 Si resonance energy and strength of an expected 3 + level in 26 Si, motivating many recent experimental studies of 26 Si structure above the proton threshold that have contributed to determining the energy and strength of this resonance but without absolutely conclusive results [4,5,6,7,8,9,10,11,12,13,14,17,18]. A 2009 evaluation [15] of available experimental data pointed out the utility of 26 P β decay for the study of this level resulting in the conclusion that it resides at a relatively precise c.m.…”