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The semi-empirical initial-final mass relation (IFMR) connectsspectroscopically analyzed white dwarfs in star clusters to the initial massesof the stars that formed them. Most current stellar evolution models, however,predict that stars will evolve to white dwarfs $\sim$0.1 M$_\odot$ less massivethan that found in the IFMR. We first look at how varying theoretical mass-lossrates, third dredge-up efficiencies, and convective-core overshoot may helpexplain the differences between models and observations. These parameters playan important role at the lowest masses (M$_{\rm initial}$ $<$ 3 M$_\odot$). Athigher masses, only convective-core overshoot meaningfully affects white dwarfmass, but alone it likely cannot explain the observed white dwarf masses norwhy the IFMR scatter is larger than observational errors predict. These highermasses, however, are also where rotational mixing in main sequence stars beginsto create more massive cores, and hence more massive white dwarfs. Thisrotational mixing also extends a star's lifetime, making faster rotatingprogenitors appear like less massive stars in their semi-empirical ageanalysis. Applying the observed range of young B-dwarf rotations to the MIST orSYCLIST rotational models demonstrates a marked improvement in reproducing boththe observed IFMR data and its scatter. The incorporation of both rotation andefficient convective-core overshoot significantly improves the match withobservations. This work shows that the IFMR provides a valuable observationalconstraint on how rotation and convective-core overshoot affect the coreevolution of a star.

A Novel Approach to Constrain Rotational Mixing & Convective-Core Overshoot in Stars Using the Initial-Final Mass Relation