  In high metallicity environments the mass that black holes (BHs) can reach
just after core-collapse widely depends on how much mass their progenitor stars
lose via winds. On one hand new theoretical and observational insights suggest
that early-stage winds should be weaker than what many canonical models
prescribe. On the other hand the proximity to the Eddington limit should affect
the formation of optically thick envelopes already during the earliest stages
of stars with initial masses $M_{\rm ZAMS}\gtrsim 100$ M$_\odot$, hence
resulting in higher mass-loss rates during the main sequence. We use the
evolutionary codes MESA and Genec to calculate a suite of tracks for massive
stars at solar metallicity Z$_\odot=0.014$ which incorporate these changes in
our wind mass loss prescription. In our calculations we employ moderate
rotation, high overshooting and magnetic angular momentum transport. We find a
maximum BH mass $M_{\rm BH, max}=28.3$ M$_\odot$ at Z$_\odot$. The most massive
BHs are predicted to form from stars with $M_{\rm ZAMS}\gtrsim 250$ M$_\odot$,
with the BH mass directly proportional to its progenitor's $M_{\rm ZAMS}$. We
also find in our models that at Z$_\odot$ almost any BH progenitor naturally
evolves into a Wolf-Rayet star due to the combined effect of internal mixing
and wind mass loss. These results are considerably different from most recent
studies regarding the final mass of stars before their collapse into BHs. While
we acknowledge the inherent uncertainties in stellar evolution modelling, our
study underscores the importance of employing the most up-to-date physics in BH
mass predictions.
