  Strong metallicity-dependent winds dominate the evolution of core He-burning,
classical Wolf-Rayet (cWR) stars, which eject both H and He-fusion products
such as 14N, 12C, 16O, 19F, 22Ne and 23Na during their evolution. The chemical
enrichment from cWRs can be significant. cWR stars are also key sources for
neutron production relevant for the weak s-process. We calculate stellar models
of cWRs at solar metallicity for a range of initial Helium star masses
(12-50M), adopting the recent hydrodynamical wind rates from Sander & Vink
(2020). Stellar wind yields are provided for the entire post-main sequence
evolution until core O-exhaustion. While literature has previously considered
cWRs as a viable source of the radioisotope 26Al, we confirm that negligible
26Al is ejected by cWRs since it has decayed to 26Mg or proton-captured to
27Al. However, in Paper I, Higgins et al. (2023) we showed that very massive
stars eject substantial quantities of 26Al, among other elements including N,
Ne, and Na, already from the zero-age-main-sequence. Here, we examine the
production of 19F and find that even with lower mass-loss rates than previous
studies, our cWR models still eject substantial amounts of 19F. We provide
central neutron densities (Nn) of a 30M cWR compared with a 32M post-VMS WR and
confirm that during core He-burning, cWRs produce a significant number of
neutrons for the weak s-process via the 22Ne(alpha,n)25Mg reaction. Finally, we
compare our cWR models with observed [Ne/He], [C/He] and [O/He] ratios of
Galactic WC and WO stars.
