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How many r-process components? A view from the mirror image of s-process studies

Published online by Cambridge University Press:  23 December 2005

R. Gallino ,
G.J. Wasserburg ,
M. Busso  and
O. Straniero
R. Gallino
Affiliation:
Dipartimento di Fisica Generale, Via P. Giuria 1, Torino 10125, Italy email: gallino@ph.unito.it
G.J. Wasserburg
Affiliation:
California Institute of Technology Pasadena (CA, USA) email: gjw@gps.caltech.edu
M. Busso
Affiliation:
Dip. Fisica, Universitá di Perugia (Italy) email: maurizio.busso@fisica.unipg.it
O. Straniero
Affiliation:
Teramo Observatory, INAF, Teramo 64100, Italy email: straniero@oa-teramo.inaf.it
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Abstract

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The classical analysis of the s-process is commonly used to predict the s percentage contribution to the solar system abundance of a given isotope, and by default of the r-process residual (calculated as 1. - s). We discuss the advantages and the disadvantages of this first-order prediction, by comparing stellar model calculations at various metallicities in AGB stars and in massive stars exploding as SNII, with spectroscopic observations of different stellar populations. Observations of short-lived r-process isotopes in the early solar system help to characterize at least three different r-process components.

Keywords

Nuclear reactionsnucleosynthesisabundancesstars: abundancesstars: AGBstars: Population II
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. 461 - 466
Copyright
© 2005 International Astronomical Union