Nucleosynthesis by the s-PROCESS in Stars of 9 and 15 Solar Masses

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Abstract

Evolutionary sequences of models of 9 and 15 Mo (solar mass) stars are combined with the details of the Ne22(a,n)Mg25 neutron-source reaction and of the neutron-capture processes to determine the abun- dances of heavy elements produced by the s-process of stellar nucleosynthesis. The central temperatures become high enough for neutron production when the convective core shrinks in mass. At the end of core helium burning, the material of the core remnant exhibits an exposure to neutrons which increases toward the center. Taking the 9 Mo model as a standard, we consider three variations: (1) a minimum- source reaction rate, (2) an increased source-to-seed ratio, and (3) an increased mass (15 Mo). Although a distribution of exposures is produced in each case, the maximum exposures are less than that of solar system material. The f(A) curves (product of the neutron-capture cross-section and of the abundance of a nuclide of atomic mass A) which would result from mixing various portions of the core remnant with unprocessed envelope material are compared with thef(A) curves of solar system material and of the Ba ii stars

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