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Mass loss is a key uncertainty in the evolution of massive stars. Stellarevolution calculations must employ parametric algorithms for mass loss, andusually only include stellar winds. We carry out a parameter study of theeffects of wind mass loss on massive star evolution using the open-sourcestellar evolution code MESA. We provide a systematic comparison of wind massloss algorithms for solar-metallicity, nonrotating, single stars in the initialmass range of $15-35\,M_\odot$. We consider combinations drawn from two hotphase algorithms, three cool phase algorithms, and two Wolf-Rayet algorithms.We consider linear wind efficiency scale factors of $1$, $0.33$, and $0.1$ toaccount for reductions in mass loss rates due to wind inhomogeneities. We findthat the initial to final mass mapping for each zero-age main-sequence (ZAMS)mass has a $\sim 50\%$ uncertainty if all algorithm combinations and windefficiencies are considered. The ad-hoc efficiency scale factor dominates thisuncertainty. While the final total mass and internal structure of our modelsvary tremendously with mass loss treatment, final observable parameters aremuch less sensitive for ZAMS mass $\lesssim 30\,M_\odot$. This indicates thatuncertainty in wind mass loss does not negatively affect estimates of the ZAMSmass of most single-star supernova progenitors from pre-explosion observations.Furthermore, we show that the internal structure of presupernova stars issensitive to variations in both main sequence and post main-sequence mass loss.We find that the compactness parameter $\xi\propto M/R(M)$ varies by as much as$30\%$ for a given ZAMS mass evolved with different wind efficiencies and massloss algorithm combinations. [abridged]

A Systematic Survey of the Effects of Wind Mass Loss Algorithms on the Evolution of Single Massive Stars