  Radioactive nuclei were present in the early Solar System, as inferred from
analysis of meteorites. Many are produced in massive stars, either during their
lives or their final explosions. In the first paper in this series (Brinkman et
al. 2019), we focused on the production of $^{26}$Al in massive binaries. Here,
we focus on the production of another two short-lived radioactive nuclei,
$^{36}$Cl and $^{41}$Ca, and the comparison to the early Solar System data. We
used the MESA stellar evolution code with an extended nuclear network and
computed massive (10-80 M$ _{\odot} $), rotating (with initial velocities of
150 and 300 km/s) and non-rotating single stars at solar metallicity (Z=0.014)
up to the onset of core collapse. We present the wind yields for the
radioactive isotopes $^{26}$Al, $^{36}$Cl, and $^{41}$Ca, and the stable
isotopes $^{19}$F and $^{20}$Ne. In relation to the stable isotopes, we find
that only the most massive models, $\geq$ 60M$_{\odot}$ and $\geq$
40M$_{\odot}$ give positive $^{19}$F and $^{20}$Ne yields, respectively,
depending on the initial rotation rate. In relation to the radioactive
isotopes, we find that the early Solar System abundances of $^{26}$Al and
$^{41}$Ca can be matched with by models with initial masses
$\geq$40M$_{\odot}$, while $^{36}$Cl is matched only by our most massive
models, $\geq$60M$_{\odot}$. $^{60}$Fe is not significantly produced by any
wind model, as required by the observations. Therefore, massive star winds are
a favoured candidate for the origin of the very short-lived $^{26}$Al,
$^{36}$Cl, and $^{41}$Ca in the early Solar System.

Solar and Stellar Astrophysics