Mean-field lattice equations of state. III. Modeling the phase behavior of supercritical gas-polymer mixtures

1990 ◽  
Vol 23 (8) ◽  
pp. 2321-2329 ◽  
Author(s):  
Eric J. Beckman ◽  
Ronald Koningsveld ◽  
Roger S. Porter
Langmuir ◽  
2002 ◽  
Vol 18 (2) ◽  
pp. 377-381 ◽  
Author(s):  
G. A. van Ewijk ◽  
G. J. Vroege

Langmuir ◽  
2003 ◽  
Vol 19 (10) ◽  
pp. 4483-4492 ◽  
Author(s):  
Nadezhda P. Shusharina ◽  
Sudhakar Balijepalli ◽  
Henri J. M. Gruenbauer ◽  
Paschalis Alexandridis

Author(s):  
Eric J. Beckman ◽  
Roger S. Porter ◽  
Ronald Koningsveld ◽  
Ludo A. Kleintjens

Universe ◽  
2019 ◽  
Vol 5 (8) ◽  
pp. 186 ◽  
Author(s):  
Mateusz Cierniak ◽  
Tobias Fischer ◽  
Niels-Uwe Bastian ◽  
Thomas Klähn ◽  
Marc Salinas

We construct a set of equations of state (EoS) of dense and hot matter with a 1st order phase transition from a hadronic system to a deconfined quark matter state. In this two-phase approach, hadrons are described using the relativistic mean field theory with different parametrisations and the deconfined quark phase is modeled using vBag, a bag–type model extended to include vector interactions as well as a simultaneous onset of chiral symmetry restoration and deconfinement. This feature results in a non–trivial connection between the hadron and quark EoS, modifying the quark phase beyond its onset density. We find that this unique property has an impact on the predicted hybrid (quark core) neutron star mass–radius relations.


2004 ◽  
Vol 13 (07) ◽  
pp. 1249-1253
Author(s):  
DÉBORA P. MENEZES ◽  
C. PROVIDÊNCIA

We investigate the properties of mixed stars formed by hadronic and quark matter in β-equilibrium described by appropriate equations of state (EOS) in the framework of relativistic mean-field theory. The calculations were performed for T=0 and for finite temperatures and also for fixed entropies with and without neutrino trapping in order to describe neutron and proto-neutron stars. The star properties are discussed. Maximum allowed masses for proto-neutron stars are much larger when neutrino trapping is imposed.


2002 ◽  
Vol 35 (14) ◽  
pp. 5630-5639 ◽  
Author(s):  
Jeffrey J. Krueger ◽  
Philip P. Simon ◽  
Harry J. Ploehn

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