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Neutron sources during shell C-burning in massive stars

Published online by Cambridge University Press:  23 December 2005

Marco Pignatari ,
R. Gallino ,
C. Baldovin  and
F. Herwig
Marco Pignatari
Affiliation:
Dipartimento di Fisica Generale, Via P. Giuria 1, Torino 10125, Italia email: pignatar@ph.unito.it, gallino@ph.unito.it, baldovin@studenti.ph.unito.it
R. Gallino
Affiliation:
Dipartimento di Fisica Generale, Via P. Giuria 1, Torino 10125, Italia email: pignatar@ph.unito.it, gallino@ph.unito.it, baldovin@studenti.ph.unito.it
C. Baldovin
Affiliation:
Dipartimento di Fisica Generale, Via P. Giuria 1, Torino 10125, Italia email: pignatar@ph.unito.it, gallino@ph.unito.it, baldovin@studenti.ph.unito.it
F. Herwig
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM 87544, USA email: fherwig@lanl.gov
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Abstract

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We present a study of the s–process nucleosynthesis (weak s-process) occurring during convective core He–burning and convective shell Carbon–burning in a massive star of 25 M$_{\odot}$. We use an updated nuclear network for the various neutron sources and for all neutron captures and β-decay rates involved. Large uncertainties affect the final yields due to the present unsatisfactory knowledge of all neutron capture cross sections involved.

Keywords

Nuclear reactionsnucleosynthesisabundancesstars: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S228: From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution , May 2005 , pp. 495 - 496
Copyright
© 2005 International Astronomical Union