An approach toward the successful supernova explosion by physics of unstable nuclei
arXiv:astro-ph/0506619 · doi:10.1016/j.nuclphysa.2005.05.017
Abstract
We study the explosion mechanism of collapse-driven supernovae by numerical simulations with a new nuclear EOS based on unstable nuclei. We report new results of simulations of general relativistic hydrodynamics together with the Boltzmann neutrino-transport in spherical symmetry. We adopt the new data set of relativistic EOS and the conventional set of EOS (Lattimer-Swesty EOS) to examine the influence on dynamics of core-collapse, bounce and shock propagation. We follow the behavior of stalled shock more than 500 ms after the bounce and compare the evolutions of supernova core.
arXiv comment4 pages, 2 figures, contribution to Nuclei in the Cosmos 8, to appear in Nucl. Phys. A
References in corpus (11)
- Relativistic Equation of State of Nuclear Matter for Supernova and Neutron Star
- Relativistic Equation of State of Nuclear Matter for Supernova Explosion
- Shock Breakout in Core-Collapse Supernovae and its Neutrino Signature
- Probing the gravitational well: No supernova explosion in spherical symmetry with general relativistic Boltzmann neutrino transport
- High Resolution Calculations of Merging Neutron Stars III: Gamma-Ray Bursts
- Spherically Symmetric Simulation with Boltzmann Neutrino Transport of Core Collapse and Post-Bounce Evolution of a 15 Solar Mass Star
- Simulation of the Spherically Symmetric Stellar Core Collapse, Bounce, and Postbounce Evolution of a 13 Solar Mass Star with Boltzmann Neutrino Transport, and Its Implications for the Supernova Mechanism
- An Implicit Lagrangean Code for Spherically Symmetric General Relativistic Hydrodynamics with an Approximate Riemann Solver
- r-Process in Prompt Supernova Explosions Revisited
- Hydrodynamical study of neutrino-driven wind as an r-process site
- Properties of a relativistic equation of state for collapse-driven supernovae