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Using the new state-of-the-art core-collapse supernova (CCSN) codeF{\sc{ornax}}, we have simulated the three-dimensional dynamical evolution ofthe cores of 9-, 10-, 11-, 12-, and 13-M$_{\odot}$ stars from the onset ofcollapse. Stars from 8-M$_{\odot}$ to 13-M$_{\odot}$ constitute roughly 50% ofall massive stars, so the explosive potential for this mass range is importantto the overall theory of CCSNe. We find that the 9-, 10-, 11-, and12-M$_{\odot}$ models explode in 3D easily, but that the 13-M$_{\odot}$ modeldoes not. From these findings, and the fact that slightly more massiveprogenitors seem to explode \citep{vartanyan2019}, we suggest that there is agap in explodability near 12-M$_{\odot}$ to 14-M$_{\odot}$ for non-rotatingprogenitor stars. Factors conducive to explosion are turbulence behind thestalled shock, energy transfer due to neutrino-matter absorption andneutrino-matter scattering, many-body corrections to the neutrino-nucleonscattering rate, and the presence of a sharp silicon-oxygen interface in theprogenitor. Our 3D exploding models frequently have a dipolar structure, withthe two asymmetrical exploding lobes separated by a pinched waist where mattertemporarily continues to accrete. This process maintains the driving neutrinoluminosty, while partially shunting matter out of the way of the expandinglobes, thereby modestly facilitating explosion. The morphology of all 3Dexplosions is characterized by multiple bubble structures with a range oflow-order harmonic modes. Though much remains to be done in CCSN theory, theseand other results in the literature suggest that, at least for these lower-massprogenitors, supernova theory is converging on a credible solution.

Three-Dimensional Supernova Explosion Simulations of 9-, 10-, 11-, 12-, and 13-M$_{\odot}$ Stars