Orateur
Description
The evolution of core-collapse supernovae (CCSNe) involves the formation and evolution of a proto-neutron star (PNS), whose structure and dynamics are strongly governed by the nuclear equation of state (EOS). In rapidly rotating CCSNe, the EOS plays a key role in setting the conditions for the onset and evolution of non-axisymmetric instabilities.
We present three-dimensional neutrino-magnetohydrodynamic simulations of the collapse of a rapidly rotating, weakly magnetised massive-star progenitor, using different finite-temperature nuclear EOSs. Despite the different EOS prescriptions, all models develop two distinct phases of non-axisymmetric corotation instabilities during the post-bounce evolution, indicating that their development is a robust feature of rapidly rotating CCSNe. However, their onset, dominant azimuthal modes, duration, and characteristic frequencies vary significantly with the EOS. These differences arise from the EOS-dependent evolution of the PNS structure, compactness, and rotation profile, which determine the conditions under which the instabilities develop and evolve.
We find that the characteristic frequencies of the instabilities correlate with the PNS compactness and tidal deformability, providing a direct link between the properties of dense nuclear matter and the dynamical behaviour of the newly formed compact object. The associated large-scale spiral modes also leave characteristic imprints on the gravitational-wave and neutrino signals. Overall, our results highlight the important role of the nuclear EOS in shaping the development and evolution of rotational instabilities in rapidly rotating CCSNe.
| Which working group does your abstract concern? | Étoiles à neutrons, supernovae et synthèse des éléments lourds / Neutron stars, supernovae and nucleosynthesis |
|---|