An Exploration of the Equation of State Dependence of Core-collapse Supernova Explosion Outcomes and Signatures
- 1Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA; [email protected]
- 2Department of Physics, University of California, Berkeley, CA 94720-7300, USA
- 3Department of Physics, University of Idaho, Moscow, ID 83843, USA
Abstract
We explore, using a state-of-the-art simulation code in 3D and late-enough times to witness final observables, the dependence of core-collapse supernova explosions on the nuclear equation of state (EOS). Going beyond questions of explodability, we compare final explosion energies, nucleosynthetic yields, recoil kicks, and gravitational-wave and neutrino signatures using the SFHo and DD2 nuclear EOSs for a 9 M ⊙ /solar-metallicity progenitor star. The DD2 EOS is stiffer and has a lower effective nucleon mass. The result is a more extended protoneutron star (PNS) and lower central densities. As a consequence, the mean neutrino energies, final explosion energy, and recoil kick speed are lower. Moreover, the evolution of PNS convection differs between the two EOS models in significant ways. This translates in part into interestingly altered neutrino “light” curves and noticeably altered gravitational-wave signal strengths and frequency characteristics that may be diagnostic. The faster exploding model (SFHo) yields slightly more neutron-rich ejecta and more species with atomic weights between 60 and 90 and a weak r -process. However, this is merely a preliminary study. The next step is a more comprehensive and multiprogenitor set of 3D supernova simulations for various EOSs to late times when the observables have asymptoted. Such a future investigation will have a direct bearing on the neutron star and black hole birth mass functions and the quest toward a fully quantitative theory of supernova observables.
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BibTeX
@article{rusakov2026exploration,
title = {{An Exploration of the Equation of State Dependence of Core-collapse Supernova Explosion Outcomes and Signatures}},
author = {Aleksandr Rusakov and Adam S. Burrows and Tianshu Wang and David Vartanyan},
journal = {The Astrophysical Journal},
year = {2026},
month = may,
doi = {10.3847/1538-4357/ae61ac},
url = {https://doi.org/10.3847/1538-4357/ae61ac},
note = {CC BY},
}
RIS
TY - JOUR
TI - An Exploration of the Equation of State Dependence of Core-collapse Supernova Explosion Outcomes and Signatures
AU - Aleksandr Rusakov
AU - Adam S. Burrows
AU - Tianshu Wang
AU - David Vartanyan
PY - 2026
DA - 2026/05/13
JO - The Astrophysical Journal
DO - 10.3847/1538-4357/ae61ac
UR - https://doi.org/10.3847/1538-4357/ae61ac
AB - We explore, using a state-of-the-art simulation code in 3D and late-enough times to witness final observables, the dependence of core-collapse supernova explosions on the nuclear equation of state (EOS). Going beyond questions of explodability, we compare final explosion energies, nucleosynthetic yields, recoil kicks, and gravitational-wave and neutrino signatures using the SFHo and DD2 nuclear EOSs for a 9 M ⊙ /solar-metallicity progenitor star. The DD2 EOS is stiffer and has a lower effective nucleon mass. The result is a more extended protoneutron star (PNS) and lower central densities. As a consequence, the mean neutrino energies, final explosion energy, and recoil kick speed are lower. Moreover, the evolution of PNS convection differs between the two EOS models in significant ways. This translates in part into interestingly altered neutrino “light” curves and noticeably altered gravitational-wave signal strengths and frequency characteristics that may be diagnostic. The faster exploding model (SFHo) yields slightly more neutron-rich ejecta and more species with atomic weights between 60 and 90 and a weak r -process. However, this is merely a preliminary study. The next step is a more comprehensive and multiprogenitor set of 3D supernova simulations for various EOSs to late times when the observables have asymptoted. Such a future investigation will have a direct bearing on the neutron star and black hole birth mass functions and the quest toward a fully quantitative theory of supernova observables.
SN - 0004-637X
SN - 1538-4357
ER -