Speaker
Marco Pignatari
(Universita' di Torino)
Description
In massive stars evolution the s-process is activated at different temperatures,
during He-burning and during C-burning.
In the convective C Shell, the s-process affects the previous Core He-burning s
yields, and the final results carry the signature of both the two following neutron
capture processes.
A detailed analysis of the s-process in massive stars is presented, in particular
at the end of the Shell C-burning when the local temperature could rapidly increase
with the s-process efficiency.
Author
Marco Pignatari
(Universita' di Torino)
Co-authors
Dr
Alexander Heger
(Los Alamos Laboratory (LANL))
Ms
Carla Baldovin
(Universita' di Torino)
Prof.
Falk Herwig
(Los Alamos Laboratory (LANL))
Prof.
Michael Wiescher
(Notre Dame University)
Prof.
Roberto Gallino
(Universita' di Torino)
