Abstract
With the (RB)-B-3-LAND setup at GSI we have measured exclusive
relative-energy spectra of the Coulomb dissociation of C-18 at a
projectile energy around 425A MeV on a lead target, which are needed to
determine the radiative neutron-capture cross sections of C-17 into the
ground state of C-18. Those data have been used to constrain theoretical
calculations for transitions populating excited states in C-18. This
allowed to derive the astrophysical cross section sigma(n gamma)*.
accounting for the thermal population of C-17 target states in
astrophysical scenarios. The experimentally verified capture rate is
significantly lower than those of previously obtained Hauser-Feshbach
estimations at temperatures T-9 <= 1 GK. Network simulations with
updated neutron-capture rates and hydrodynamics according to the
neutrino-driven wind model as well as the neutron-star merger scenario
reveal no pronounced influence of neutron capture of C-17 on the
production of second-and third-peak elements in contrast to earlier
sensitivity studies.
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