Fluctuation effects in hot quark matter: Precursors of chiral transition at finite temperature

1985 ◽  
Vol 55 (2) ◽  
pp. 158-161 ◽  
Author(s):  
T. Hatsuda ◽  
T. Kunihiro
Keyword(s):  
Quark Matter ◽  
Finite Temperature ◽  
Chiral Transition ◽  
Fluctuation Effects ◽  
Hot Quark Matter

scholarly journals Chiral Symmetry Restoration for Quark Matter with a Chiral Chemical Potential

2017 ◽  
Vol 45 ◽  
pp. 1760044 ◽  
Author(s):  
Ricardo L. S. Farias ◽  
Dyana C. Duarte ◽  
Gastão Krein ◽  
Rudnei O. Ramos
Keyword(s):  
Chiral Symmetry ◽  
Quark Matter ◽  
Finite Temperature ◽  
Chemical Potential ◽  
Separation Scheme ◽  
Chiral Symmetry Restoration ◽  
Chiral Transition

In this work we study the chiral transition in quark matter at finite temperature and in the presence of a chiral imbalance in the Nambu–Jona-Lasinio model. We use the Medium Separation Scheme (MSS) to rewrite divergent momentum integrals that appear in the model in such way that we can conciliate results obtained with the model and recent lattice results for the chiral transition.

scholarly journals Light Front Approach to Correlations in Hot Quark Matter

2006 ◽  
Vol 27 (2-3) ◽  
pp. 379-382
Author(s):  
S. Strauß ◽  
M. Beyer ◽  
S. Mattiello
Keyword(s):  
Quark Matter ◽  
Light Front ◽  
Hot Quark Matter

FINITE TEMPERATURE EQUATIONS OF STATE FOR MIXED STARS

2004 ◽  
Vol 13 (07) ◽  
pp. 1249-1253
Author(s):  
DÉBORA P. MENEZES ◽  
C. PROVIDÊNCIA
Keyword(s):  
Field Theory ◽  
Neutron Stars ◽  
Quark Matter ◽  
Finite Temperature ◽  
Equations Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Relativistic Mean Field Theory ◽  
Relativistic Mean Field

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.

STAR: Characterizing hot quark matter

2013 ◽  
Author(s):  
G. Van Buren ◽  
STAR Collaboration
Keyword(s):  
Quark Matter ◽  
Hot Quark Matter
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