A Finite Difference Representation of Neutrino Radiation Hydrodynamics in Spherically Symmetric General Relativistic Space-Time
M. Liebendoerfer,O. E. B. Messer,Anthony Mezzacappa,S. W. Bruenn,Christian Y. Cardall,Friedrich-Karl Thielemann +5 more
TLDR
Agile Boltztran as discussed by the authors solves the Boltzmann transport equation for the angular and spectral neutrino distribution functions in self-consistent simulations of stellar core collapse and postbounce evolution.Abstract:
We present an implicit finite difference representation for general relativistic radiation hydrodynamics in spherical symmetry. Our code, Agile-Boltztran, solves the Boltzmann transport equation for the angular and spectral neutrino distribution functions in self-consistent simulations of stellar core collapse and postbounce evolution. It implements a dynamically adaptive grid in comoving coordinates. Most macroscopically interesting physical quantities are defined by expectation values of the distribution function. We optimize the finite differencing of the microscopic transport equation for a consistent evolution of important expectation values. We test our code in simulations launched from progenitor stars with 13 solar masses and 40 solar masses. ~0.5 s after core collapse and bounce, the protoneutron star in the latter case reaches its maximum mass and collapses further to form a black hole. When the hydrostatic gravitational contraction sets in, we find a transient increase in electron flavor neutrino luminosities due to a change in the accretion rate. The muon- and tauon-neutrino luminosities and rms energies, however, continue to rise because previously shock-heated material with a non-degenerate electron gas starts to replace the cool degenerate material at their production site. We demonstrate this by supplementing the concept of neutrinospheres with a more detailed statistical description of the origin of escaping neutrinos. We compare the evolution of the 13 solar mass progenitor star to simulations with the MGFLD approximation, based on a recently developed flux limiter. We find similar results in the postbounce phase and validate this MGFLD approach for the spherically symmetric case with standard input physics.read more
Citations
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Journal ArticleDOI
Explosion Mechanisms of Core-Collapse Supernovae
TL;DR: The neutrino-heating mechanism, aided by nonradial flows, drives explosions, albeit low-energy ones, of O-Ne-Mg-core and some Fe-core progenitors as mentioned in this paper.
Journal ArticleDOI
Black hole formation in failing core-collapse supernovae
Evan O'Connor,Christian D. Ott +1 more
TL;DR: In this article, the authors present results of a systematic study of failing core-collapse supernovae and the formation of stellar-mass black holes (BHs) using GR1D equipped with a three-species neutrino leakage/heating scheme.
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Core-collapse supernova equations of state based on neutron star observations
TL;DR: In this paper, a spherically symmetric core-collapse supernova model based on general relativistic radiation hydrodynamics with three-flavor Boltzmann neutrino transport is proposed.
Journal ArticleDOI
Protoneutron star evolution and the neutrino-driven wind in general relativistic neutrino radiation hydrodynamics simulations
Tobias Fischer,S. C. Whitehouse,Anthony Mezzacappa,Friedrich-Karl Thielemann,Matthias Liebendörfer +4 more
TL;DR: In this paper, a spherically symmetric general relativistic radiation hydrodynamics using spectral three-flavor Boltzmann neutrino transport is used to simulate the collapse, bounce, explosion, and the neutrini-driven wind phases consistently over more than 20 s.
Journal ArticleDOI
Physics of Core-Collapse Supernovae in Three Dimensions: a Sneak Preview
TL;DR: The first successful neutrino-driven supernova explosion was obtained with self-consistent, first-principle simulations in three spatial dimensions (3D).
References
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Book
Computational Methods of Neutron Transport
Elmer E Lewis,W. F. Miller +1 more
TL;DR: In this paper, a balanced overview of the major methods currently available for obtaining numerical solutions in neutron and gamma ray transport is presented, focusing on methods particularly suited to the complex problems encountered in the analysis of reactors, fusion devices, radiation shielding, and other nuclear systems.