出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：The radioactive nucleus 60Fe has been recently detected in the Galaxy for the first time, with
the RHESSI (Reuven Ramaty High Energy Solar Spectroscopic Imager) satellite and with the
SPI spectrometer onboard INTEGRAL (International Gamma-Ray Astrophysics Laboratory). In
addition, galactic emission from 26Al has been confirmed and observed with excellent energetic
resolution with these two missions. In the light of these advances, an analysis of these two radioactive
isotopes and the g-ray line flux ratio between them is presented, under the assumption
that massive stars are the sole contributors. We discuss the range of uncertainty of the yields
derived from theoretical stellar models and focus on the influence of metallicity on them. Comparison
between theoretical and observed 60Fe/26Al flux ratios is a potential tool to claim a global
need of extra sources of 26Al, as well as to discard or support some prescriptions for the mass loss
rate affecting the ejection of the synthesized 26Al and 60Fe into the interstellar medium. However,
the broad range of theoretical 60Fe/26Al ratios obtained prevents to extract accurate constraints on
theoretical models of massive stars.
