Comparison of the Core-collapse Evolution of Two Nearly Equal-mass Progenitors

We compare the core-collapse evolution of a pair of 15.8 M-? stars with significantly different internal structures, a consequence of the bimodal variability exhibited by massive stars during their late evolutionary stages. The 15.78 and 15.79 M-? progenitors have core masses (masses interior to an entropy of 4 k (B) baryon(-1)) of 1.47 and 1.78 M-? and compactness parameters ?(1.75) of 0.302 and 0.604, respectively. The core-collapse simulations are carried out in 2D to nearly 3 s postbounce and show substantial differences in the times of shock revival and explosion energies. The 15.78 M-? model begins exploding promptly at 120 ms postbounce when a strong density decrement at the Si-Si/O shell interface, not present in the 15.79 M-? progenitor, encounters the stalled shock. The 15.79 M-? model takes 100 ms longer to explode but ultimately produces a more powerful explosion. Both the larger mass accretion rate and the more massive core of the 15.79 M-? model during the first 0.8 s postbounce time result in larger ?(e )/? over bar e M (?) model resulted in the ejection of twice as much Ni-56. Most of the ejecta in both models are moderately proton rich, though counterintuitively the highest electron fraction (Y-e = 0.61) ejecta in either model are in the less-energetic 15.78 M-? model, while the lowest electron fraction (Y-e = 0.45) ejecta in either model are in the 15.79 M-? model.