Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12-25 M_sol Stars

TL;DR

This study presents axisymmetric ab initio supernova simulations for 12-25 solar mass stars, demonstrating shock revival driven by neutrino heating, with results indicating potential explosions and energies comparable to observed supernovae.

Contribution

First detailed axisymmetric supernova simulations with spectral neutrino transport across multiple progenitor masses, showing shock revival and explosion energies.

Findings

Shock revival occurs within ~200 ms post-bounce.

Progenitors of 12-20 M_sol can fully unbind their envelopes.

Explosion energies range from 0.33 to 0.70 Bethe, increasing over time.

Abstract

We present an overview of four ab initio axisymmetric core-collapse supernova simulations employing detailed spectral neutrino transport computed with our CHIMERA code and initiated from Woosley & Heger (2007) progenitors of mass 12, 15, 20, and 25 M_sol. All four models exhibit shock revival over \sim 200 ms (leading to the possibility of explosion), driven by neutrino energy deposition. Hydrodynamic instabilities that impart substantial asymmetries to the shock aid these revivals, with convection appearing first in the 12 M_sol model and the standing accretion shock instability (SASI) appearing first in the 25 M_sol model. Three of the models have developed pronounced prolate morphologies (the 20 M_sol model has remained approximately spherical). By 500 ms after bounce the mean shock radii in all four models exceed 3,000 km and the diagnostic explosion energies are 0.33, 0.66, 0.65, and 0.70 Bethe (B = $10^{51}$ ergs) for the 12, 15, 20, and 25 M_sol models, respectively, and are increasing. The three least massive of our models are already sufficiently energetic to completely unbind the envelopes of their progenitors (i.e., to explode), as evidenced by our best estimate of their explosion energies, which first become positive at 320, 380, and 440 ms after bounce. By 850 ms the 12 M_sol diagnostic explosion energy has saturated at 0.38 B, and our estimate for the final kinetic energy of the ejecta is \sim 0.3 B, which is comparable to observations for lower-mass progenitors.