SURVEY OF CORE-COLLAPSE SNe FROM 9 to 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONSCollaborators: Thomas Ertl, Stan Woosley, Justin Brown, Thomas Janka
Status: submitted to The Astrophysical Journal
Fig. 12 of SEWBJ (2015). The explosion outcomes are shown for five different 'engines' calibrated to SN1987A. Engines are listed in increasing strength.
In Sukhbold & Woosley (2014), we have explored in detail the systematics of presupernova core structure as a function of initial mass, using a number of fine-meshed surveys. The variation of the core compactness with mass is found to be robustly non-monotonic and is heavily dependent on the complex interplay of shell burning episodes during the advanced stages of evolution. In this work, we are studying the explosion outcomes of 200 progenitor models between 9-120Msun through a novel approach. Instead of placing the piston in an arbitrary location and dial-in the final kinetic energy at infinity, we first create series of calibrated (to SN1987A and SN1054 observations) ''engines'' from the combination of one-zone analytic core-cooling model and approximate neutrino-transport. Then we place these engines inside each progenitor, and follow the evolution until the remnant and ejecta are clearly separated (neutrino-radiation hydrodynamics is calculated with Prometheus-HOTB as described in Ertl et al. 2015). Once we give up the luxury of exploding any star in any way we want, now the outcomes are based on the neutrino-driven mechanism and therefore heavily dependent on the progenitor structure - i.e. each successful explosion for each engine has a different energy, remnant mass and nucleosynthesis. As predicted in prior work on progenitors, most stars explode below 20Msun with significant modulation, and above there is a sea of black hole formation with a distinct island of explosion near 27Msun. We map the explosion results back into KEPLER to post-process the resulting nucleosynthesis (excluding r-process but including Type-Ia contribution) with a large network, and follow the light curves through flux-limited diffusion.