A numerical method for solving the neutrino Boltzmann equation coupled to spherically symmetric stellar core collapse

1993 ◽  
Vol 405 ◽  
pp. 669 ◽  
Author(s):  
Anthony Mezzacappa ◽  
Stephen W. Bruenn
Keyword(s):  
Boltzmann Equation ◽  
Numerical Method ◽  
Core Collapse ◽  
Spherically Symmetric ◽  
Stellar Core

scholarly journals 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

2001 ◽  
Vol 86 (10) ◽  
pp. 1935-1938 ◽  
Author(s):  
Anthony Mezzacappa ◽  
Matthias Liebendörfer ◽  
O. E. Bronson Messer ◽  
W. Raphael Hix ◽  
Friedrich-Karl Thielemann ◽  
...  
Keyword(s):  
Core Collapse ◽  
Spherically Symmetric ◽  
Stellar Core

scholarly journals Gravitational wave extraction in simulations of rotating stellar core collapse

2011 ◽  
Vol 83 (6) ◽  
Author(s):  
C. Reisswig ◽  
C. D. Ott ◽  
U. Sperhake ◽  
E. Schnetter
Keyword(s):  
Gravitational Wave ◽  
Core Collapse ◽  
Stellar Core

scholarly journals Stellar Core Collapse and Exotic Matter

2011 ◽  
Vol 7 (S279) ◽  
pp. 367-368
Author(s):  
Ken'ichiro Nakazato ◽  
Kohsuke Sumiyoshi
Keyword(s):  
Black Hole ◽  
Degrees Of Freedom ◽  
Gamma Ray ◽  
Dense Matter ◽  
Gamma Ray Bursts ◽  
Core Collapse ◽  
Hole Formation ◽  
Stellar Core ◽  
Black Hole Formation ◽  
Hydrodynamical Simulations

AbstractSome supernovae and gamma-ray bursts are thought to accompany a black hole formation. In the process of a black hole formation, a central core becomes hot and dense enough for hyperons and quarks to appear. In this study, we perform neutrino-radiation hydrodynamical simulations of a stellar core collapse and black hole formation taking into account such exotic components. In our computation, general relativity is fully considered under spherical symmetry. As a result, we find that the additional degrees of freedom soften the equation of state of matter and promote the black hole formation. Furthermore, their effects are detectable as a neutrino signal. We believe that the properties of hot and dense matter at extreme conditions are essential for the studies on the astrophysical black hole formation. This study will be hopefully a first step toward a physics of the central engine of gamma-ray bursts.

scholarly journals The antesonic condition for the explosion of core-collapse supernovae – I. Spherically symmetric polytropic models: stability and wind emergence

2018 ◽  
Vol 481 (3) ◽  
pp. 3293-3304 ◽  
Author(s):  
Matthias J Raives ◽  
Sean M Couch ◽  
Johnny P Greco ◽  
Ondřej Pejcha ◽  
Todd A Thompson
Keyword(s):  
Core Collapse ◽  
Spherically Symmetric

Experimental limit to the Galactic stellar core collapse based on the Baksan scintillation telescope data 1980–1993

1994 ◽  
Vol 35 ◽  
pp. 270-272 ◽  
Author(s):  
E.N. Alexeyev ◽  
L.N. Alexeyeva ◽  
A.E. Chudakov ◽  
G.D. Korotkii ◽  
N.A. Metlinskii ◽  
...  
Keyword(s):  
Core Collapse ◽  
Experimental Limit ◽  
Stellar Core

Stellar core collapse. I - Infall epoch

1981 ◽  
Vol 249 ◽  
pp. 270 ◽  
Author(s):  
K. A. van Riper ◽  
J. M. Lattimer
Keyword(s):  
Core Collapse ◽  
Stellar Core

scholarly journals Physical, numerical, and computational challenges of modeling neutrino transport in core-collapse supernovae

2020 ◽  
Vol 6 (1) ◽  
Author(s):  
Anthony Mezzacappa ◽  
Eirik Endeve ◽  
O. E. Bronson Messer ◽  
Stephen W. Bruenn
Keyword(s):  
Phase Space ◽  
Weak Interactions ◽  
Kinetic Equations ◽  
Distribution Functions ◽  
Core Collapse ◽  
Algebraic Equations ◽  
Stellar Core ◽  
Dimensional Phase Space ◽  
Solution Methods ◽  
Physical Laws

AbstractThe proposal that core collapse supernovae are neutrino driven is still the subject of active investigation more than 50 years after the seminal paper by Colgate and White. The modern version of this paradigm, which we owe to Wilson, proposes that the supernova shock wave is powered by neutrino heating, mediated by the absorption of electron-flavor neutrinos and antineutrinos emanating from the proto-neutron star surface, or neutrinosphere. Neutrino weak interactions with the stellar core fluid, the theory of which is still evolving, are flavor and energy dependent. The associated neutrino mean free paths extend over many orders of magnitude and are never always small relative to the stellar core radius. Thus, neutrinos are never always fluid like. Instead, a kinetic description of them in terms of distribution functions that determine the number density of neutrinos in the six-dimensional phase space of position, direction, and energy, for both neutrinos and antineutrinos of each flavor, or in terms of angular moments of these neutrino distributions that instead provide neutrino number densities in the four-dimensional phase-space subspace of position and energy, is needed. In turn, the computational challenge is twofold: (i) to map the kinetic equations governing the evolution of these distributions or moments onto discrete representations that are stable, accurate, and, perhaps most important, respect physical laws such as conservation of lepton number and energy and the Fermi–Dirac nature of neutrinos and (ii) to develop efficient, supercomputer-architecture-aware solution methods for the resultant nonlinear algebraic equations. In this review, we present the current state of the art in attempts to meet this challenge.

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