Progress on nuclear reaction rates affecting the stellar production of <SUP>26</SUP>Al

Abstract

The radioisotope <SUP>26</SUP>Al is a key observable for nucleosynthesis in the Galaxy and the environment of the early Solar System. To properly interpret the large variety of astronomical and meteoritic data, it is crucial to understand both the nuclear reactions involved in the production of <SUP>26</SUP>Al in the relevant stellar sites and the physics of such sites. These range from the winds of low- and intermediate-mass asymptotic giant branch stars; to massive and very massive stars, both their Wolf-Rayet winds and their final core-collapse supernovae (CCSN); and the ejecta from novae, the explosions that occur on the surface of a white dwarf accreting material from a stellar companion. Several reactions affect the production of <SUP>26</SUP>Al in these astrophysical objects, including (but not limited to) <SUP>25</SUP>Mg(p, γ)<SUP>26</SUP>Al, <SUP>26</SUP>Al(p, γ)<SUP>27</SUP>Si, and <SUP>26</SUP>Al(n, p/α). Extensive experimental effort has been spent during recent years to improve our understanding of such key reactions. Here we present a summary of the astrophysical motivation for the study of <SUP>26</SUP>Al, a review of its production in the different stellar sites, and a timely evaluation of the currently available nuclear data. We also provide recommendations for the nuclear input into stellar models and suggest relevant, future experimental work.