scholarly journals Extended equation of state for core-collapse simulations

2012 ◽  
Vol 85 (5) ◽  
Author(s):  
M. Oertel ◽  
A. F. Fantina ◽  
J. Novak
Keyword(s):  
Equation Of State ◽  
Core Collapse ◽  
Extended Equation Of State

An Extended Equation of State Modeling Method II. Mixtures

2006 ◽  
Vol 27 (5) ◽  
pp. 1319-1353 ◽  
Author(s):  
G. Scalabrin ◽  
P. Marchi ◽  
P. Stringari ◽  
D. Richon
Keyword(s):  
Equation Of State ◽  
Modeling Method ◽  
Extended Equation Of State

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 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

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.

scholarly journals Equation of state effects in the core collapse of a 20−M⊙ star

2019 ◽  
Vol 100 (5) ◽  
Author(s):  
A. S. Schneider ◽  
L. F. Roberts ◽  
C. D. Ott ◽  
E. O'Connor
Keyword(s):  
Equation Of State ◽  
Core Collapse ◽  
The Core
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