Speaker
Description
Core-collapse supernovae (CCSNe) are among the most energetic phenomena in the Universe and are promising multimessenger sources of gravitational waves (GWs) and neutrinos. The nuclear equation of state (EOS) is a key ingredient in CCSN simulations, as it determines the thermodynamic properties of dense matter, the structure and maximum mass of the proto-neutron star (PNS), and consequently the dynamics of the explosion and its multimessenger signatures.
We present three-dimensional neutrino magnetohydrodynamic simulations of the collapse of a rapidly rotating, weakly magnetised 35 M$_\odot$ progenitor performed with five different finite-temperature nuclear EOSs. Despite the different EOS prescriptions, all models develop two similar phases of non-axisymmetric corotation instabilities within the first 1.25 s after core bounce, suggesting that their occurrence is a robust feature largely independent of the EOS. However, the onset time, dominant azimuthal mode, lifetime, and characteristic multimessenger frequencies differ significantly among the models, reflecting EOS-dependent variations in the evolving PNS structure and rotation profile. The resulting large-scale spiral modes produce quasi-periodic GW emission and modulate the neutrino luminosities. The characteristic GW frequencies associated with both instabilities correlate with the PNS compactness and tidal deformability, with stiffer PNSs producing higher-frequency emission. Finally, the EOS strongly influences the overall morphological evolution of otherwise identical models, highlighting its fundamental role in shaping the dynamics and multimessenger signals of rapidly rotating CCSNe.