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We present the evolution of massive star progenitors of supernovae of typeIIP. We take the example of the nearby and well-studied SN 2013ej. We explorehow convective overshoot affects the stellar structure, surface abundances, andeffective temperature of massive stars, using the Modules for Experiments inStellar Astrophysics (MESA). In particular models with moderate overshoot ($f$= 0.02 to 0.031) show the presence of blue loops in the Hertzsprung-Russelldiagram with a red to blue [$log_{10}(T_{eff}/\rm K)$ from $< 3.6$ to $> 4.0$]excursion and transition back to red, during core helium burning phase. Modelswith overshoot outside this range of $f$ values kept the star in the redsupergiant state throughout the post helium ignition phases. The surface CNOabundance shows enrichment post-main-sequence and again around the time whenhelium is exhausted in core. These evolutionary changes in surface CNOabundance are indistinguishable in the currently available observations due tolarge observational uncertainties. However, these observations may distinguishbetween the ratios of surface nitrogen to oxygen at different evolutionarystages of the star. We also compare the effects of convective overshoot onvarious parameters related to likelihood of explosion of a star as opposed tocollapse to a black hole. These parameters are the compactness parameter,M$_4$, and $\mu_4$. Combination $\mu_4 \times $M$_4$, and $\mu_4$ have similarvariation with $f$ and both peak out at $f$ = 0.032. We find that all of our 13M$_{\odot}$ models are likely to explode.

Type IIP Supernova Progenitors and their explodability I: Convective Overshoot, Blue Loops and Surface Composition