scholarly journals Equation of state for nuclear matter in relativistic mean-field theory and Maxwellian phase transition to strange quark matter

2012 ◽  
Author(s):  
Grigor Alaverdyan
Keyword(s):  
Field Theory ◽  
Phase Transition ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Quark Matter ◽  
Strange Quark ◽  
Mean Field Theory ◽  
Mean Field ◽  
Strange Quark Matter ◽  
Relativistic Mean Field

HADRON-QUARK PHASE TRANSITION AND ANTIKAON CONDENSATION IN NEUTRON STARS

2008 ◽  
Vol 23 (27n30) ◽  
pp. 2481-2484
Author(s):  
H. SHEN ◽  
F. YANG ◽  
P. YUE
Keyword(s):  
Field Theory ◽  
Phase Transition ◽  
Equation Of State ◽  
Neutron Stars ◽  
Mean Field Theory ◽  
Mean Field ◽  
Maximum Mass ◽  
Relativistic Mean Field ◽  
The Core ◽  
Quark Phase

We study the hadron-quark phase transition and antikaon condensation which may occur in the core of massive neutron stars. The relativistic mean field theory is used to describe the hadronic phase, while the Nambu-Jona-Lasinio model is adopted for the quark phase. We find that the hadron-quark phase transition is very sensitive to the models used. The appearance of deconfined quark matter and antikaon condensation can soften the equation of state at high density and lower the maximum mass of neutron stars.

HOT NUCLEAR MATTER PROPERTIES

2007 ◽  
Vol 16 (09) ◽  
pp. 3041-3044
Author(s):  
TOMAZ PASSAMANI ◽  
MARIA LUIZA CESCATO
Keyword(s):  
Field Theory ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Finite Temperature ◽  
Mean Field Theory ◽  
Mean Field ◽  
Nonlinear Interactions ◽  
Nucleon Mass ◽  
Relativistic Mean Field ◽  
Linear And Nonlinear

The nuclear matter at finite temperature is described in the relativistic mean field theory using linear and nonlinear interactions. The behavior of effective nucleon mass with temperature was numerically calculated. For the nonlinear NL3 interaction we also observed the striking decrease at temperatures well below the nucleon mass. The calculation of NL3 nuclear matter equation of state at finite temperature is still on progress.

scholarly journals PHASE TRANSITION AND HYBRID STAR IN A NONLINEAR σ–ω MODEL

1999 ◽  
Vol 08 (02) ◽  
pp. 107-120 ◽  
Author(s):  
S. ACHARYA ◽  
L. MAHARANA ◽  
R. MOHANTY ◽  
P. K. PANDA
Keyword(s):  
Phase Transition ◽  
Nuclear Matter ◽  
Quark Matter ◽  
Equations Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Coupling Constant ◽  
Hybrid Star ◽  
Relativistic Mean Field ◽  
Outer Periphery

The phase transition between nuclear matter and quark matter is examined. The relativistic mean field theory (RMF) is considered with interacting nucleons and mesons using TM1 parameter set for the nuclear matter equations of state. It is found that the transition point depends on coupling constant αs and bag pressure. From the study of the structure of a hybrid neutron star, it is observed that the star contains quark matter in the interior and neutron matter on the outer periphery.

IMPORTANCE OF THE π-FIELD IN THE RELATIVISTIC MEAN FIELD THEORY FOR NUCLEAR MATTER

1995 ◽  
Vol 10 (37) ◽  
pp. 2809-2818 ◽  
Author(s):  
QI-REN ZHANG ◽  
WALTER GREINER
Keyword(s):  
Field Theory ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Mean Field Theory ◽  
Mean Field ◽  
Relativistic Mean Field Theory ◽  
Relativistic Mean Field ◽  
Nuclear Equation Of State ◽  
Walecka Model

We generalize the Walecka model for nuclear matter by including the π-field. It is found that a finite mean π-field may lower the energy per nucleon even in the nuclear matter of subnormal density. A mean π-field may significantly change the nuclear equation of state. The importance of considering the π-field in the relativistic mean field theory for nuclear matter is therefore emphasized.

EFFECT OF MAGNETIC FIELD ON THE PHASE TRANSITION FROM NUCLEAR MATTER TO QUARK MATTER DURING PROTO-NEUTRON STAR EVOLUTION

2002 ◽  
Vol 11 (04) ◽  
pp. 545-559 ◽  
Author(s):  
V. K. GUPTA ◽  
ASHA GUPTA ◽  
S. SINGH ◽  
J. D. ANAND
Keyword(s):  
Magnetic Field ◽  
Phase Transition ◽  
Quark Matter ◽  
Mean Field Theory ◽  
Mean Field ◽  
Relativistic Mean Field ◽  
Electron Neutrinos ◽  
Hadron Phase ◽  
Frame Work ◽  
Trapped Electron

We have studied phase transition from hadron matter to quark matter in the presence of high magnetic fields incorporating the trapped electron neutrinos at finite temperatures. We have used the density dependent quark mass (DDQM) model for the quark phase while the hadron phase is treated in the frame-work of relativistic mean field theory. It is seen that the energy density in the hadron phase at phase transition decreases with both magnetic field and temperature.

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.

scholarly journals Kaon condensation and equation of state in the relativistic mean-field theory

1994 ◽  
Vol 337 (1-2) ◽  
pp. 19-24 ◽  
Author(s):  
Tomoyuki Maruyama ◽  
Hirotsugu Fujii ◽  
Takumi Muto ◽  
Toshitaka Tatsumi
Keyword(s):  
Field Theory ◽  
Equation Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Relativistic Mean Field Theory ◽  
Relativistic Mean Field ◽  
Kaon Condensation
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