(26)Aluminum from Massive Binary Stars. II. Rotating Single Stars Up to Core Collapse and Their Impact on the Early Solar System

Radioactive nuclei were present in the early solar system (ESS), as inferred from analysis of meteorites. Many are produced in massive stars, either during their lives or their final explosions. In the first paper of this series (Brinkman et al. 2019), we focused on the production of Al-26 in massive binaries. Here, we focus on the production of another two short-lived radioactive nuclei, Cl-36 and Ca-41, and the comparison to the ESS data. We used the MESA stellar evolution code with an extended nuclear network and computed massive (10-80 M (circle dot)), rotating (with initial velocities of 150 and 300 km s(-1)) and nonrotating single stars at solar metallicity (Z = 0.014) up to the onset of core collapse. We present the wind yields for the radioactive isotopes Al-26, Cl-36, and Ca-41, and the stable isotopes F-19 and Ne-22. In relation to the stable isotopes, we find that only the most massive models, >= 60 and >= 40 M (circle dot) give positive F-19 and Ne-22 yields, respectively, depending on the initial rotation rate. In relation to the radioactive isotopes, we find that the ESS abundances of Al-26 and Ca-41 can be matched with by models with initial masses >= 40 M (circle dot), while Cl-36 is matched only by our most massive models, >= 60 M (circle dot). Fe-60 is not significantly produced by any wind model, as required by the observations. Therefore, massive star winds are a favored candidate for the origin of the very short-lived Al-26, Cl-36, and Ca-41 in the ESS.