2D and 3D core-collapse supernovae simulation results obtained with the CHIMERA code

Much progress in realistic modeling of core-collapse supernovae has occurred recently through the availability of multi-teraflop machines and the increasing sophistication of supernova codes. These improvements are enabling simulations with enough realism that the explosion mechanism, long a mystery, may soon be delineated. We briefly describe the CHIMERA code, a supernova code we have developed to simulate core-collapse supernovae in 1, 2, and 3 spatial dimensions. We then describe the results of an ongoing suite of 2D simulations initiated from a 12, 15, 20, and 25 solar mass progenitor. These have all exhibited explosions and are currently in the expanding phase with the shock at between 5,000 and 20,000 km. We also briefly describe an ongoing simulation in 3 spatial dimensions initiated from the 15 solar mass progenitor.

[1]  M. Rampp,et al.  Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport - I. Numerical method and results for a 15 solar mass star , 2005, astro-ph/0507135.

[2]  Richard H. White,et al.  The Hydrodynamic Behavior of Supernovae Explosions , 1964 .

[3]  L. Scheck,et al.  Neutrino-driven Convection versus Advection in Core-Collapse Supernovae , 2005, astro-ph/0507636.

[4]  E. Müller,et al.  Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions , 2006, astro-ph/0601302.

[5]  A. Mezzacappa,et al.  Stability of Standing Accretion Shocks, with an Eye toward Core-Collapse Supernovae , 2002, astro-ph/0210634.

[6]  S. E. Woosley,et al.  Nucleosynthesis and remnants in massive stars of solar metallicity , 2007 .

[7]  M. Rampp,et al.  Supernova Simulations with Boltzmann Neutrino Transport: A Comparison of Methods , 2003, astro-ph/0310662.

[8]  Anthony Mezzacappa,et al.  Probing the gravitational well: no supernova explosion in spherical symmetry with general relativistic boltzmann neutrino transport , 2001 .

[9]  P. Woodward,et al.  The Piecewise Parabolic Method (PPM) for Gas Dynamical Simulations , 1984 .

[10]  W. R. Hix,et al.  Computational methods for nucleosynthesis and nuclear energy generation , 1999 .

[11]  H. A. Bethe,et al.  Supernova mechanisms. [SN 1987a] , 1990 .

[12]  R. Peletier.  PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE , 2009 .

[13]  O. E. B. Messer,et al.  A Finite Difference Representation of Neutrino Radiation Hydrodynamics in Spherically Symmetric General Relativistic Spacetime , 2002 .

[14]  R. Sutherland,et al.  The Numerical Simulation of Radiative Shocks. I. The Elimination of Numerical Shock Instabilities Using a Local Oscillation Filter , 2002, astro-ph/0204373.

[15]  A. Mezzacappa,et al.  Simulation of the spherically symmetric stellar core collapse, bounce, and postbounce evolution of a star of 13 solar masses with boltzmann neutrino transport, and its implications for the supernova mechanism. , 2000, Physical review letters.

[16]  F. Thielemann,et al.  Astrophysical reaction rates from statistical model calculations , 2000, astro-ph/0004059.

[17]  Non-spherical core collapse supernovae - II. The late-time evolution of globally anisotropic neutrino-driven explosions and their implications for SN 1987 A , 2005, astro-ph/0511369.