Modeling core collapse supernovae in 2 and 3 dimensions with spectral neutrino transport

Abstract

The overwhelming evidence that the core collapse supernova mechanism is inherently multidimensional, the complexity of the physical processes involved, and the increasing evidence from simulations that the explosion is marginal presents great computational challenges for the realistic modeling of this event, particularly in 3 spatial dimensions. We have developed a code which is scalable to computations in 3 dimensions which couples PPM Lagrangian with remap hydrodynamics [1], multigroup, flux-limited diffusion neutrino transport [2], with many improvements), and a nuclear network [3]. The neutrino transport is performed in a ray-by-ray plus approximation wherein all the lateral effects of neutrinos are included (e.g., pressure, velocity corrections, advection) except the transport. A moving radial grid option permits the evolution to be carried out from initial core collapse with only modest demands on the number of radial zones. The inner part of the core is evolved after collapse along with the rest of the core and mantle by subcycling the lateral evolution near the center as demanded by the small Courant times. We present results of 2-D simulations of a symmetric and an asymmetric collapse of both a 15 and an 11 M progenitor. In each of these simulations we have discovered that once the oxygen rich material reaches the shock there is a synergistic interplay between the reduced ram pressure, the energy released by the burning of the shock heated oxygen rich material, and the neutrino energy deposition which leads to a revival of the shock and an explosion.

arXiv comment10 pages, 3 figures

References in corpus (11)

• Astrophysical Reaction Rates From Statistical Model Calculations
• Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport. I. Numerical method and results for a 15 M_sun star
• A New Mechanism for Core-Collapse Supernova Explosions
• Neutrino Interactions in Hot and Dense Matter
• Non-spherical Core Collapse Supernovae I. Neutrino-Driven Convection, Rayleigh-Taylor Instabilities, and the Formation and Propagation of Metal Clumps
• A Finite Difference Representation of Neutrino Radiation Hydrodynamics in Spherically Symmetric General Relativistic Space-Time
• Supernova Neutrino Opacity from Nucleon-Nucleon Bremsstrahlung and Related Processes
• The Spherical Accretion Shock Instability in the Linear Regime
• Neutrino and axion emissivities of neutron stars from nucleon-nucleon scattering data
• Simulating Self-gravitating Hydrodynamic Flows
• General Relativistic Effects in the Core Collapse Supernova Mechanism

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