Multicomponent hard-sphere heterochain fluid: equations of state in a continuum space

1992 ◽  
Vol 25 (23) ◽  
pp. 6262-6269 ◽  
Author(s):  
A. O. Malakhov ◽  
E. B. Brun
1996 ◽  
Vol 100 (2) ◽  
pp. 928-928
Author(s):  
Richard J. Sadus

1991 ◽  
Vol 32 (8) ◽  
pp. 2258-2262 ◽  
Author(s):  
D. Wang ◽  
L. R. Mead ◽  
M. de Llano

2015 ◽  
Vol 29 (13) ◽  
pp. 1550089 ◽  
Author(s):  
Minhui Shan ◽  
Jianxiang Tian

As is well-known, the structures and thermodynamic properties of fluids are determined by the complex interactions, i.e., the repulsive one and the attractive one, among particles. The simplest equation-of-state (EOS) model maybe the one of hard sphere repulsion plus or multiplying some attraction. Followed by the rapid promotion of the accuracy of hard sphere EOS in the past dozens of years, one question rises as whether more accurate hard sphere repulsion derives better prediction of the structures and properties of fluids with a special attraction. In this work, we used two repulsions with clearly different accuracy and some attractions to construct series equations of state (EOSs) for real fluids, and then we discussed the saturated properties at liquid–gas equilibrium. We found that the answer to the question aforementioned is not definitely standing.


1991 ◽  
Vol 30 (1) ◽  
pp. 39-42 ◽  
Author(s):  
M.J. Maeso ◽  
J.R. Solana ◽  
J. Amorós ◽  
E. Villar

1999 ◽  
Vol 110 (11) ◽  
pp. 5444-5457 ◽  
Author(s):  
G. Stell ◽  
C.-T. Lin ◽  
Yu. V. Kalyuzhnyi

2003 ◽  
Vol 12 (03) ◽  
pp. 519-526 ◽  
Author(s):  
J. E. HORVATH ◽  
G. LUGONES ◽  
J. A. DE FREITAS PACHECO

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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