Hydrodynamic instabilities in long-term three-dimensional simulations of neutrino-driven supernovae of 13 red supergiant progenitors
- 1Universitat de Valéncia Departamento de Astronomía y Astrofísica, , E-46100 Burjassot (Valéncia) ,
- 2Max-Planck-Institute for Astrophysics , Karl-Schwarzschild-Str. 1, 85748 Garching ,
Abstract
We present long-term three-dimensional (3D) simulations of Type-IIP supernovae (SNe) for 13 non-rotating, single-star, red-supergiant (RSG) progenitors with zero-age-main-sequence masses between 12.5 M⊙ and 27.3 M⊙. The explosions were modelled with a parametric treatment of neutrino heating to obtain defined energies, 56Ni yields, and neutron-star properties in agreement with previous results. Our 3D SN models were evolved from core bounce until 10 days to study how the large-scale mixing of chemical elements depends on the progenitor structure. Rayleigh-Taylor instabilities (RTIs), which grow at the (C+O)/He and He/H interfaces and interact with the reverse shock forming after the SN shock has passed the He/H interface, play a crucial role in the outward mixing of 56Ni into the hydrogen envelope. We find most extreme 56Ni mixing and the highest maximum 56Ni velocities in lower-mass (LM) explosions despite lower explosion energies, and the weakest 56Ni mixing in the 3D explosions of the most massive RSGs. The efficiency of radial 56Ni mixing anti-correlates linearly with the helium-core mass and correlates positively with the magnitude of a local maximum of ρr3 in the helium shell. This maximum causes shock deceleration and therefore facilitates high growth factors of RTI at the (C+O)/He interface in the LM explosions. Therefore fast-moving 56Ni created by the asymmetric neutrino-heating mechanism is carried into the ubiquitous RT-unstable region near the He/H interface and ultimately far into the envelopes of the exploding RSGs. Our correlations may aid improving mixing prescriptions in 1D SN models and deducing progenitor structures from observed SN properties.
Related
- Three-dimensional circumplanetary flows in a PDS 70c-inspired system: hydrodynamic simulations with FARGO3D and analysis with FARGOpy
- Binary Progenitors of Electron-capture Supernovae
- Binary Progenitors of Electron-capture Supernovae
- It Takes Two: nucleosynthesis in core-collapse supernova simulations of binary-star progenitors
- Charged-current neutrino opacity within the relativistic Hartree-Fock framework for astrophysical simulations of core-collapse supernovae and binary neutron star mergers
BibTeX
@article{giudici2026hydrodynamic,
title = {{Hydrodynamic instabilities in long-term three-dimensional simulations of neutrino-driven supernovae of 13 red supergiant progenitors}},
author = {B. Giudici and Michael Gabler and Hans‐Thomas Janka},
journal = {Monthly Notices of the Royal Astronomical Society},
year = {2026},
month = oct,
doi = {10.1093/mnras/stag1978},
url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1978/8943788},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Hydrodynamic instabilities in long-term three-dimensional simulations of neutrino-driven supernovae of 13 red supergiant progenitors
AU - B. Giudici
AU - Michael Gabler
AU - Hans‐Thomas Janka
PY - 2026
DA - 2026/10/19
JO - Monthly Notices of the Royal Astronomical Society
DO - 10.1093/mnras/stag1978
UR - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1978/8943788
AB - We present long-term three-dimensional (3D) simulations of Type-IIP supernovae (SNe) for 13 non-rotating, single-star, red-supergiant (RSG) progenitors with zero-age-main-sequence masses between 12.5 M⊙ and 27.3 M⊙. The explosions were modelled with a parametric treatment of neutrino heating to obtain defined energies, 56Ni yields, and neutron-star properties in agreement with previous results. Our 3D SN models were evolved from core bounce until 10 days to study how the large-scale mixing of chemical elements depends on the progenitor structure. Rayleigh-Taylor instabilities (RTIs), which grow at the (C+O)/He and He/H interfaces and interact with the reverse shock forming after the SN shock has passed the He/H interface, play a crucial role in the outward mixing of 56Ni into the hydrogen envelope. We find most extreme 56Ni mixing and the highest maximum 56Ni velocities in lower-mass (LM) explosions despite lower explosion energies, and the weakest 56Ni mixing in the 3D explosions of the most massive RSGs. The efficiency of radial 56Ni mixing anti-correlates linearly with the helium-core mass and correlates positively with the magnitude of a local maximum of ρr3 in the helium shell. This maximum causes shock deceleration and therefore facilitates high growth factors of RTI at the (C+O)/He interface in the LM explosions. Therefore fast-moving 56Ni created by the asymmetric neutrino-heating mechanism is carried into the ubiquitous RT-unstable region near the He/H interface and ultimately far into the envelopes of the exploding RSGs. Our correlations may aid improving mixing prescriptions in 1D SN models and deducing progenitor structures from observed SN properties.
SN - 0035-8711
SN - 1365-2966
SN - 1365-8711
ER -