3D numerical study of magnetorotational effects on extreme core-collapse supernovae

by Liubov Kovalenko (Stockholm University)

Wednesday 17 Dec 2025, 11:00 → 12:00 Europe/Stockholm

Albano 3: 6228 - Mega (22 seats) (Albano Building 3)

Core-collapse supernovae are among the most energetic explosions in the universe. Their evolution is shaped by the hydrodynamics, neutrino transport, and magnetic fields at work in the first seconds after the collapse. We investigate these processes through 3D simulations of an extremely compact 39-Msun progenitor using the FLASH M1 magnetohydrodynamics code. Our study explores three models – a nonmagnetized nonrotating baseline model, a nonmagnetized rotating model, and a magnetized rotating model – to highlight the roles of rotation and magnetic fields in shaping the explosion mechanism and multi-messenger signals. We evolve each model from core collapse through bounce and into the early post-bounce phase (~0.7s post-bounce). We use a three-species, energy-dependent M1 moment scheme for neutrino transport, incorporating a state-of-the-art nuclear equation of state and advanced treatments of deleptonization and neutrino heating/cooling. All three simulations undergo similar gravitational collapse and bounces. During the post-bounce phase, rotation and magnetic fields significantly impact the shock dynamics, explosion morphology, protoneutron star development, and angular variations in neutrino distributions. We will present these findings, highlighting how rotation and magnetization influence neutrino and GW signatures. We will discuss potential observational signatures that could help distinguish magnetorotationally influenced explosions from more spherical cases. Future work will refine our treatment of neutrino microphysics and magnetic fields while extending simulations to longer time scales and a broader range of progenitor conditions.