出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：A comparative analysis of the various scenarios proposed to explain the 26Al content of the galaxy,
as observed through its characterisitc g -ray line at 1.8 MeV, is presented. We include some suggestions
about how theoretical yields should be handled, accounting for the influence of the initial
metallicity of the corresponding star, which depends not only on its mass but also on its location
in the galaxy. A code of chemical evolution of the galaxy is used to derive the temporal evolution
of metallicity along the galaxy, the necessary tool to determine the initial metallicity of any stellar
source of 26Al. The contribution of each scenario (AGB stars, massive stars and classical novae)
and its range of uncertainty are described.
