Liubov Kovalenko: Rotation and Magnetic Fields in Extreme Core-Collapse Supernovae
A5:1003
AlbaNova Main Building
Core-collapse supernovae are shaped by the interplay of gravity, neutrinos, rotation, and magnetic fields in the first seconds after collapse. While most simulations focus on neutrino-driven hydrodynamics, magnetic fields are likely essential for understanding the most rapidly rotating and extreme explosions, as well as their connection to magnetar formation.
In this talk, I will present 3D simulations of an extremely compact 39-solar-mass progenitor and compare three models: a non-rotating baseline case, a rotating case without magnetic fields, and a rotating magnetized case. Although the collapse and bounce are broadly similar, the post-bounce evolution differs significantly. Rotation and magnetic fields alter the shock evolution, outflow morphology, proto-neutron-star dynamics, and the angular structure of the neutrino emission.
These differences are especially important for multimessenger signals. Because the newly formed core is initially opaque to photons (and even neutrinos), gravitational waves may provide the earliest direct observational window into the proto-neutron star just after bounce. Using these models, I will discuss how rotation and magnetic fields influence both the explosion dynamics and the gravitational-wave signatures that may provide access to the innermost post-bounce evolution.