出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：The main-s process component, which produces the s abundances from Sr to Pb/Bi, occurs in
low-mass thermally pulsing AGB stars. In this scenario, the 13C(a
n)16O reaction, which burns
radiatively at T
0
9
108 K during the interpulse period, constitutes the major neutron source.
A second weaker neutron source, the 22Ne(a
n)25Mg, is partially activated during the convective
thermal pulses, when the maximum temperature at the bottom of the He-burning shell reaches a
value of T
3
108 K. Using improved stellar (n
g ) cross sections and stellar AGB models with
a full reaction network we report on an updated reproduction of the solar main-s component.
We also present the status of a measurement of the 209Bi(n,g )210Big cross section, which aims at
reducing the uncertainties to about 2%, and improving the accuracy of the abundances prediction
at the termination point of the s
path.
