The88Sr(p,γ)89Yreaction at astrophysically relevant energies

Experimentally constrained(p,γ)Y89and(n,γ)Larsen1, Guttormsen2, Schwengner3 et al. 2016Phys. Rev. CSelf Cite334241View full textAdd to dashboardCite

“…For the 88 Sr(p, γ) 89 Y cross section, direct measurements exist [63]. Overall, we find a very good agreement between our calculations and the 88 Sr(p, γ) 89 Y data from Ref.…”

“…For the γSF data, we have tuned the γSF models to reproduce our lower and upper data points. Specifically, we have used a low-lying M1 strength that cor- [63], and the corresponding astrophysical reaction rates (b) compared to the BRUSLIB (dashed magenta line, Ref. [50]) and the JINA REACLIB (green solid line, Ref.…”

The [sup 85]Rb(p,n)[sup 85]Sr reaction and the modified proton optical potential

“…The relevant astrophysical reaction rates can be determined from the cross section of the inverse capture reactions through the detailed balance theorem if the corresponding capture cross sections are known experimentally. In the last few years several proton capture cross section measurements for p process studies were carried out [5,6,7,8,9,10,11,12,13,14,15,16,17,18,19,20]. However, it has been shown recently that not only (γ,p) reactions are important for modeling the synthesis of the light p nuclei, but (n,p) and (p,n) reactions should also be taken into account [4].…”

Proton capture reaction cross section measurements on Er162 as a probe of statistical model calculations

“…The corresponding cross section, calculated with the TALYS reaction code [17], is between 10 −8 and 10 −3 b respectively. The bulk of (p,γ ) measurements have been performed in the lower mass region (A < 112) [20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36], except for 120 Te [37], 130 Ba [38], and 152 Gd [39]. For the (p,n) channel, very few (p,n) measurements have been performed, with the exception of 76 Ge [20], 82 Se [21], 85 Rb [34], 120 Te [37], 130 Ba [38], and 152 Gd [39].…”