scholarly journals Medium modifications for light and heavy nuclear clusters in simulations of core collapse supernovae: Impact on equation of state and weak interactions

2020 ◽  
Vol 102 (5) ◽  
Author(s):  
Tobias Fischer ◽  
Stefan Typel ◽  
Gerd Röpke ◽  
Niels-Uwe F. Bastian ◽  
Gabriel Martínez-Pinedo
Keyword(s):  
Equation Of State ◽  
Weak Interactions ◽  
Core Collapse ◽  
Nuclear Clusters ◽  
Medium Modifications

A new equation of state with light nuclei and their weak interactions in core-collapse supernova simulations

2014 ◽  
Author(s):  
Shun Furusawa ◽  
Hiroki Nagakura ◽  
Kohsuke Sumiyoshi ◽  
Shoichi Yamada ◽  
Hideyuki Suzuki
Keyword(s):  
Equation Of State ◽  
Weak Interactions ◽  
Light Nuclei ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
New Equation

scholarly journals A new equation of state for core-collapse supernovae based on realistic nuclear forces and including a full nuclear ensemble

2017 ◽  
Vol 44 (9) ◽  
pp. 094001 ◽  
Author(s):  
S Furusawa ◽  
H Togashi ◽  
H Nagakura ◽  
K Sumiyoshi ◽  
S Yamada ◽  
...  
Keyword(s):  
Equation Of State ◽  
Core Collapse ◽  
Nuclear Forces ◽  
New Equation

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.

scholarly journals Equation of State Effects in Core-Collapse Supernovae

2020 ◽  
Vol 124 (9) ◽  
Author(s):  
H. Yasin ◽  
S. Schäfer ◽  
A. Arcones ◽  
A. Schwenk
Keyword(s):  
Equation Of State ◽  
Core Collapse

scholarly journals GRAVITATIONAL COLLAPSE AND WEAK INTERACTIONS

1966 ◽  
Vol 44 (11) ◽  
pp. 2553-2594 ◽  
Author(s):  
W. David Arnett
Keyword(s):  
General Relativity ◽  
Energy Transfer ◽  
Equation Of State ◽  
Gravitational Collapse ◽  
Massive Star ◽  
Weak Interactions ◽  
Approximation Procedure ◽  
The Core ◽  
Numerical Hydrodynamics ◽  
Subsequent Behavior

The behavior of a massive star during its final catastrophic stages of evolution has been investigated theoretically, with particular emphasis upon the effect of electron-type neutrino interactions. The methods of numerical hydrodynamics, with coupled energy transfer in the diffusion approximation, were used. In this respect, this investigation differs from the work of Colgate and White (1964) in which a "neutrino deposition" approximation procedure was used. Gravitational collapse initiated by electron capture and by thermal disintegration of nuclei in the stellar center is examined, and the subsequent behavior does not depend sensitively upon which process causes the collapse.As the density and temperature of the collapsing stellar core increase, the material becomes opaque to electron-type neutrinos and energy is transferred by these neutrinos to regions of the star less tightly bound by gravity. Ejection of the outer layers of the star can result. This phenomenon has been identified with supernovae.Uncertainty concerning the equation of state of a hot, dense nucleon gas causes uncertainty in the temperature of the collapsing matter. This affects the rate of energy transfer by electron-type neutrinos and the rate of energy lost to the star by muon-type neutrinos.The effects of general relativity do not appear to become important in the core until after the ejection of the outer layers.

Equation of state of dense matter for core-collapse supernovae, compact objects and neutrino bursts

2008 ◽  
Author(s):  
Kohsuke Sumiyoshi ◽  
Takuma Suda ◽  
Takaya Nozawa ◽  
Akira Ohnishi ◽  
Kiyoshi Kato ◽  
...  
Keyword(s):  
Equation Of State ◽  
Dense Matter ◽  
Compact Objects ◽  
Core Collapse

scholarly journals The State of Matter in Simulations of Core-Collapse supernovae—Reflections and Recent Developments

2017 ◽  
Vol 34 ◽  
Author(s):  
Tobias Fischer ◽  
Niels-Uwe Bastian ◽  
David Blaschke ◽  
Mateusz Cierniak ◽  
Matthias Hempel ◽  
...  
Keyword(s):  
Equation Of State ◽  
Degrees Of Freedom ◽  
The State ◽  
Core Collapse ◽  
Heavy Nuclei ◽  
Isospin Asymmetry ◽  
Wide Range ◽  
Recent Developments ◽  
State Of Matter

AbstractIn this review article, we discuss selected developments regarding the role of the equation of state in simulations of core-collapse supernovae. There are no first-principle calculations of the state of matter under supernova conditions since a wide range of conditions is covered, in terms of density, temperature, and isospin asymmetry. Instead, model equation of state are commonly employed in supernova studies. These can be divided into regimes with intrinsically different degrees of freedom: heavy nuclei at low temperatures, inhomogeneous nuclear matter where light and heavy nuclei coexist together with unbound nucleons, and the transition to homogeneous matter at high densities and temperatures. In this article, we discuss each of these phases with particular view on their role in supernova simulations.

GRAVITATIONAL COLLAPSE OF MASSIVE STARS AS A PROBE INTO HOT DENSE MATTER

2008 ◽  
Vol 23 (27n30) ◽  
pp. 2443-2450 ◽  
Author(s):  
SHOICHI YAMADA
Keyword(s):  
Equation Of State ◽  
Gravitational Collapse ◽  
Nuclear Physics ◽  
Massive Stars ◽  
Dense Matter ◽  
High Energy ◽  
Compact Objects ◽  
Core Collapse ◽  
Accretion Shock ◽  
Very High

Nuclear physics is an indispensable input for the investigation of high energy astrophysical phenomena involving compact objects. In this paper I take a gravitational collapse of massive stars as an example and show how the macroscopic dynamics is influenced by the properties of nuclei and nuclear matter. I will discuss two topics that are rather independent of each other. The first one is the interplay of neutrino-nuclei inelastic scatterings and the standing accretion shock instability in the core of core collapse supernovae and the second is concerning the neutrino emissions from black hole formations and their dependence on the equation of state at very high densities. In the latter, I will also demonstrate that future astronomical observations might provide us with valuable information on the equation of state of hot dense matter.

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