scholarly journals Impact of the Nuclear Equation of State on the Stability of Hybrid Neutron Stars

Universe ◽  
2019 ◽  
Vol 5 (8) ◽  
pp. 186 ◽  
Author(s):  
Mateusz Cierniak ◽  
Tobias Fischer ◽  
Niels-Uwe Bastian ◽  
Thomas Klähn ◽  
Marc Salinas
Keyword(s):  
Equations Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Type Model ◽  
Two Phase ◽  
Relativistic Mean Field ◽  
Nuclear Equation Of State ◽  
Hot Matter ◽  
The Stability ◽  
Quark Phase

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.

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.

GROUND STATE PROPERTIES OF SUPERHEAVY NUCLEI IN RELATIVISTIC MEAN FIELD THEORY

2006 ◽  
Vol 15 (07) ◽  
pp. 1613-1624
Author(s):  
H. F. ZHANG ◽  
J. Q. LI ◽  
W. ZUO ◽  
X. H. ZHOU ◽  
Z. G. GAN ◽  
...  
Keyword(s):  
Mean Field Theory ◽  
Mean Field ◽  
Decay Chain ◽  
Stable Region ◽  
Bcs Theory ◽  
Heavy Nuclei ◽  
Relativistic Mean Field ◽  
The Stability ◽  
Super Heavy Nuclei ◽  
The Continuum

In the framework of the relativistic mean field (RMF) theory, the stability and ground properties of super-heavy nuclei are discussed. Our study indicated that the current synthesized super-heavy nuclei (SHN) actually appear in the stable region, and adding more neutrons will not increase their stability. The study of nuclei from 287115 α decay chain showed that they are usually deformed, the magnitudes of their shell gaps are much smaller than those of nuclei before the actinium region, so that the shell effect is weakened, and SHN are usually not stable. A common phenomenon is that the Fermi surface of the proton is close to the continuum, the resonant continuums exist in SHN, because the SHN are usually neutron deficient. Although bulk properties can be described by the RMF+BCS theory, further study is needed. Density dependent delta pairing interaction can improve the treatment of the pairing and thus improve the level distribution in the continuum.

EFFECTS OF TEMPERATURE ON THE STABILITY OF PROTONEUTRON STARS WITH HYPERONS

2012 ◽  
Vol 27 (02) ◽  
pp. 1250008 ◽  
Author(s):  
ZI YU ◽  
WENBO DING ◽  
NINGNING LIU ◽  
QING LUO
Keyword(s):  
Mean Field Theory ◽  
Mean Field ◽  
Mass Range ◽  
Relativistic Mean Field ◽  
Sn 1987A ◽  
Higher Temperature ◽  
Effects Of Temperature ◽  
The Stability ◽  
Protoneutron Stars ◽  
Protoneutron Star

In the framework of the relativistic mean field theory, the stability of thermal protoneutron stars is investigated. There is a highest possible temperature for a stable protoneutron star. A stable protoneutron star may be a metastable one if its mass is too large. As the temperature increases, the metastable mass range of protoneutron stars narrows. With the increase of temperature, the probability that a stable protoneutron star is a metastable one increases. A really stable protoneutron star with higher temperature can contain more species of hyperons. The case of SN 1987A is analyzed connected with the results in this article.

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.

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.

scholarly journals Nuclear equation of state from the nonlinear relativistic mean field theory

1988 ◽  
Vol 38 (2) ◽  
pp. 1003-1009 ◽  
Author(s):  
B. M. Waldhauser ◽  
J. A. Maruhn ◽  
H. Stöcker ◽  
W. Greiner
Keyword(s):  
Field Theory ◽  
Equation Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Relativistic Mean Field Theory ◽  
Relativistic Mean Field ◽  
Nuclear Equation Of State
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