Equation of State Models

2010 ◽  
pp. 260-338
Author(s):  
Klaus Lucas
Keyword(s):  
Equation Of State ◽  
State Models

scholarly journals Development of uncertainty-aware equation-of-state models: Application to copper

2020 ◽  
Vol 128 (18) ◽  
pp. 185902
Author(s):  
S. J. Ali ◽  
D. C. Swift ◽  
C. J. Wu ◽  
R. G. Kraus
Keyword(s):  
Equation Of State ◽  
State Models

Direct detection of double retrograde behavior in binary systems for equation of state models

2016 ◽  
Vol 426 ◽  
pp. 131-144
Author(s):  
J.I. Ramello ◽  
J.M. Milanesio ◽  
G.O. Pisoni ◽  
M. Cismondi ◽  
M.S. Zabaloy
Keyword(s):  
Equation Of State ◽  
Binary Systems ◽  
Direct Detection ◽  
State Models

Making equation of state models predictive

2007 ◽  
Vol 258 (1) ◽  
pp. 41-50 ◽  
Author(s):  
Kai Leonhard ◽  
Nguyen Van Nhu ◽  
Klaus Lucas
Keyword(s):  
Equation Of State ◽  
State Models

scholarly journals QUARK–DIQUARK EQUATIONS OF STATE MODELS: THE ROLE OF INTERACTIONS

2003 ◽  
Vol 12 (03) ◽  
pp. 519-526 ◽  
Author(s):  
J. E. HORVATH ◽  
G. LUGONES ◽  
J. A. DE FREITAS PACHECO
Keyword(s):  
Equation Of State ◽  
Boundary Conditions ◽  
Neutron Stars ◽  
Hard Sphere ◽  
Degrees Of Freedom ◽  
Equations Of State ◽  
Compact Star ◽  
Star Models ◽  
State Models

Recent observational data suggests a high compacticity (the quotient M/R) of some "neutron" stars. Motivated by these works we revisit models based on quark–diquark degrees of freedom and address the question of whether that matter is stable against diquark disassembling and hadronization within the different models. We find that equations of state modeled as effective λϕ4 theories do not generally produce stable self-bound matter and are not suitable for constructing very compact star models, that is the matter would decay into neutron matter. We also discuss some insights obtained by including hard sphere terms in the equation of state to model repulsive interactions. We finally compare the resulting equations of state with previous models and emphasize the role of the boundary conditions at the surface of compact self-bound stars, features of a possible normal crust of the latter and related topics.

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