  1D stellar evolution calculations produce uncertain predictions for
quantities like the age, core mass, core compactness, and nucleo-synthetic
yields; a key source of uncertainty is the modeling of interfaces between
regions that are convectively stable and those that are not. Theoretical and
numerical work has demonstrated that there should be numerous processes
adjacent to the convective boundary that induce chemical and angular momentum
transport, as well as modify the thermal structure of the star. One such
process is called convective penetration, wherein vigorous convection extends
beyond the nominal convective boundary and alters both the composition and
thermal structure. In this work, we incorporate the process of convective
penetration in stellar evolution calculations using the stellar evolution
software instrument mesa. We implement convective penetration according to the
description presented by Anders et al. (2022a) to calculate a grid of models
from the pre main sequence to He core depletion. The extent of the convective
penetration zone is self-consistently calculated at each time step without
introducing new free parameters. We find both a substantial penetration zone in
all models with a convective core and observable differences to global stellar
properties such as the luminosity and radius. We preset how the predicted
radial extent of the penetration zone scales with the total stellar mass, age
and the metallicity of the star. We discuss our results in the context of
existing numerical and observational studies.
