Neutron radiative-capture cross-sections for «s-process » calculations in stars

Neutron Cross Sections for Nucleosynthesis Studies

“…In addition to the activation technique, the very high neutron fluxes available at spallation neutron sources appear to be promising options for such measurements [43,44]. From a list of possible measurements, priority should be given to the important branch points 79 Se, 147 Pm, 151 Sm, 163 Ho, 170 Tm, 171 Tm, 179 Ta, 204 Tl, and 205 Pb. These cases are of immediate relevance to s-process analyses and should not present unexpected experimental problems.…”

S-process studies in the light of new experimental cross sections - Distribution of neutron fluences and r-process residuals

“…Where only theoretical values exist, the uncertainties were determined by the same procedure; but even if agreement between various calculations was found, a minimum error of + 30% is assumed for these species because theoretical calculations cannot be made with better accuracy. Presently, there are four sets of theoretically calculated cross sections by Holmes et al (1976), , Harris (1981), and by Benzi, D'Orazi, and Reffo (1973) which are all based on the statistical model. While the first three sets of data werecalculated with a global set of nuclear parameters such as level densities and radiative decay widths, in the fourth work, mass dependent variations of these parameters were also considered.…”

“…(4) Benzi, d'Orazi, and Reffo (1973), + Woosley et al (19789, + Holmes et al (1976), **Harris (1981)…”

“…5.7 + 0.9 43.9 + 0.8 24.22 + 0.25 (5) 68 11 + 2 1.5 *Benzi, d'Orazi, andReffo (1973), +Leugers et al (1979) + +Holmes et al (1976( ), §Harris (1981 References to measurements: (1) Fogelberg and Macklin (1981), 2Musgrove, , (3) Siddappa, Murty, and' Rao (1973), (4) , 5 Macklin and Halperin (1976). Approximate~-process abundances derived as the difference between solar abundances (Cameron 1981) and calculated sprocess abundances.…”