scholarly journals A new equation of state with abundances of all nuclei in core collapse simulations of massive stars

2013 ◽  
Author(s):  
Shun Furusawa ◽  
K. Sumiyoshi ◽  
Shoichi Yamada ◽  
Hideyuki Suzuki
Keyword(s):  
Equation Of State ◽  
Massive Stars ◽  
Core Collapse ◽  
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

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.

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

EQUATION OF STATE OF DENSE MATTER FOR CORE-COLLAPSE SUPERNOVAE AND NEUTRINO BURSTS

2008 ◽  
Vol 23 (27n30) ◽  
pp. 2451-2454
Author(s):  
KOHSUKE SUMIYOSHI
Keyword(s):  
Black Hole ◽  
Equation Of State ◽  
Numerical Simulations ◽  
Gravitational Collapse ◽  
Massive Stars ◽  
Dense Matter ◽  
Core Collapse ◽  
Many Body ◽  
Recent Developments ◽  
Supernova Explosions

We report the recent developments on the tables of equation of state for dense matter and their influence on core-collapse supernovae and associated neutrino emissions. We study the gravitational collapse of massive stars by the numerical simulations with the tables of equation of state recently developed in relativistic many body frameworks. I discuss whether the equation of state of dense matter can be probed by the properties of neutrino signals from black hole forming supernovae, being different from ordinary neutrino bursts from supernova explosions.

scholarly journals A new equation of state Based on Nuclear Statistical Equilibrium for Core-Collapse Simulations

2011 ◽  
Vol 7 (S279) ◽  
pp. 333-334
Author(s):  
Shun Furusawa ◽  
Shoichi Yamada ◽  
Kohsuke Sumiyoshi ◽  
Hideyuki Suzuki
Keyword(s):  
Free Energy ◽  
Equation Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Statistical Equilibrium ◽  
Core Collapse ◽  
Average Mass ◽  
Relativistic Mean Field ◽  
Model Free ◽  
New Equation

AbstractWe calculate a new equation of state for baryons at sub-nuclear densities for the use in core-collapse simulations of massive stars. The formulation is the nuclear statistical equilibrium description and the liquid drop approximation of nuclei. The model free energy to minimize is calculated by relativistic mean field theory for nucleons and the mass formula for nuclei with atomic number up to ~ 1000. We have also taken into account the pasta phase. We find that the free energy and other thermodynamical quantities are not very different from those given in the standard EOSs that adopt the single nucleus approximation. On the other hand, the average mass is systematically different, which may have an important effect on the rates of electron captures and coherent neutrino scatterings on nuclei in supernova cores.

Algorithms for Density, Potential Temperature, Conservative Temperature, and the Freezing Temperature of Seawater

2006 ◽  
Vol 23 (12) ◽  
pp. 1709-1728 ◽  
Author(s):  
David R. Jackett ◽  
Trevor J. McDougall ◽  
Rainer Feistel ◽  
Daniel G. Wright ◽  
Stephen M. Griffies
Keyword(s):  
Thermal Expansion ◽  
Equation Of State ◽  
Thermodynamic Potential ◽  
Potential Temperature ◽  
Inverse Function ◽  
Freezing Temperature ◽  
Ocean Models ◽  
The Difference ◽  
New Equation ◽  
Density Equation

Abstract Algorithms are presented for density, potential temperature, conservative temperature, and the freezing temperature of seawater. The algorithms for potential temperature and density (in terms of potential temperature) are updates to routines recently published by McDougall et al., while the algorithms involving conservative temperature and the freezing temperatures of seawater are new. The McDougall et al. algorithms were based on the thermodynamic potential of Feistel and Hagen; the algorithms in this study are all based on the “new extended Gibbs thermodynamic potential of seawater” of Feistel. The algorithm for the computation of density in terms of salinity, pressure, and conservative temperature produces errors in density and in the corresponding thermal expansion coefficient of the same order as errors for the density equation using potential temperature, both being twice as accurate as the International Equation of State when compared with Feistel’s new equation of state. An inverse function relating potential temperature to conservative temperature is also provided. The difference between practical salinity and absolute salinity is discussed, and it is shown that the present practice of essentially ignoring the difference between these two different salinities is unlikely to cause significant errors in ocean models.

A New Equation of State for Fluids

1928 ◽  
Vol 63 (5) ◽  
pp. 229 ◽  
Author(s):  
James A. Beattie ◽  
Oscar C. Bridgeman
Keyword(s):  
Equation Of State ◽  
New Equation

scholarly journals A NEW EQUATION OF STATE

1929 ◽  
Vol 15 (1) ◽  
pp. 11-18 ◽  
Author(s):  
H. J. Brennen
Keyword(s):  
Equation Of State ◽  
New Equation

scholarly journals A shallow water analogue of asymmetric core-collapse, and neutron star kick/spin

2011 ◽  
Vol 7 (S279) ◽  
pp. 134-137
Author(s):  
Thierry Foglizzo ◽  
Frédéric Masset ◽  
Jérôme Guilet ◽  
Gilles Durand
Keyword(s):  
Neutron Star ◽  
Shallow Water ◽  
Acoustic Waves ◽  
Large Scale ◽  
Massive Stars ◽  
Core Collapse ◽  
Hydraulic Jumps ◽  
Core Collapse Supernova ◽  
Accretion Shock

AbstractMassive stars end their life with the gravitational collapse of their core and the formation of a neutron star. Their explosion as a supernova depends on the revival of a spherical accretion shock, located in the inner 200km and stalled during a few hundred milliseconds. Numerical simulations suggest that the large scale asymmetry of the neutrino-driven explosion is induced by a hydrodynamical instability named SASI. Its non radial character is able to influence the kick and the spin of the resulting neutron star. The SWASI experiment is a simple shallow water analog of SASI, where the role of acoustic waves and shocks is played by surface waves and hydraulic jumps. Distances in the experiment are scaled down by a factor one million, and time is slower by a factor one hundred. This experiment is designed to illustrate the asymmetric nature of core-collapse supernova.

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