Computational Challenges with Modeling Core Collapse Supernovae - IPAM at UCLA

Explore the computational challenges of modeling core collapse supernovae and their gravitational wave emission in this comprehensive lecture by Anthony Mezzacappa from the University of Tennessee. Delve into the progress made in understanding the explosion mechanism across progenitor characteristics and predicting supernova observables. Examine the need for advanced three-dimensional general relativistic neutrino-magnetohydrodynamics models with spectral or Boltzmann kinetics, incorporating relevant neutrino interactions and nuclear equations of state. Discover the complexities of developing discretizations and solution methods that satisfy Fermi-Dirac statistics, lepton number conservation, and energy conservation simultaneously. Investigate the challenges in optimizing code and the importance of continued model improvements across a larger population of progenitors. Gain insights into the efforts to achieve predictive capability in modeling core collapse supernova gravitational wave emission, including discussions on neutrino-driven convection, turbulence, sloshing, magnetic fields, and weak interaction physics.

Introduction
Its a good time to be a supernova modeler
Overview
Guardian Angel
Delayed Shock Mechanism
neutrino driven convection
turbulence
sloshing
magnetic fields
general relativistic
neutrino heating
neutrino distribution function
Eddington factor
Realizability
Where we are
Weak interaction physics
First 3D model
Explosion energy vs time
gravitational wave signatures