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.

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.

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.

A RELATIVISTIC MEAN FIELD THEORY FOR NUCLEAR MATTER AT T≠0

2004 ◽  
Vol 13 (07) ◽  
pp. 1177-1181
Author(s):  
ALEXANDRE MESQUITA ◽  
MOISÉS RAZEIRA ◽  
CÉSAR A. Z. VASCONCELLOS ◽  
MANFRED DILLIG ◽  
BARDO E. J. BODMANN
Keyword(s):  
Nuclear Matter ◽  
Mean Field Theory ◽  
Mean Field ◽  
Dense Matter ◽  
Baryon Number ◽  
Coupling Constants ◽  
Model Parameters ◽  
Static Properties ◽  
Relativistic Mean Field ◽  
Protoneutron Stars

We study effects of temperature in hadron dense matter within a generalized relativistic mean field approach based on the naturalness of the various coupling constants of the theory, The Lagrangian density of our formulation contains the fundamental baryon octet, nonlinear self-couplings of the σ and δ meson fields coupled to the baryons and to the ω and ρ meson fields. By adjusting the model parameters, after inclusion in a consistent way of chemical equilibrium, baryon number and electric charge conservation, our model describes static bulk properties of ordinary nuclear matter and neutron stars. In the framework of the Sommerfeld approximation, we extend our approach to the T≠0 domain. The Sommerfeld approximation allows a drastic simplification of computational work while improving the capability of the theoretical analysis of the role of temperature on static properties of protoneutron stars. We perform the calculations by using our nonlinear model, which we extend by considering trapped neutrinos introduced into the formalism by fixing the lepton fraction. Integrating the Tolman–Oppenheimer–Volkoff equations we have obtained standard plots for the mass and radius of protoneutron stars as a function of the central density and temperature. Our predictions include the determination of an absolute value for the protoneutron star limiting mass at low and intermediate temperature regimes.

scholarly journals Protoneutron star in the relativistic mean-field theory

2001 ◽  
Vol 27 (9) ◽  
pp. 1917-1938 ◽  
Author(s):  
R Manka ◽  
M Zastawny-Kubica ◽  
A Brzezina ◽  
I Bednarek
Keyword(s):  
Field Theory ◽  
Mean Field Theory ◽  
Mean Field ◽  
Relativistic Mean Field Theory ◽  
Relativistic Mean Field ◽  
Protoneutron Star

scholarly journals Property difference between the neutron star PSR J0348+0432 and its proto neutron star

2017 ◽  
Vol 26 (11) ◽  
pp. 1750133 ◽  
Author(s):  
Xian-Feng Zhao
Keyword(s):  
Neutron Star ◽  
Mean Field Theory ◽  
Mean Field ◽  
Baryon Number ◽  
Particle Number Density ◽  
Number Density ◽  
Hyperon Production ◽  
Relativistic Mean Field ◽  
Higher Temperature ◽  
Proto Neutron Star

The property difference between the neutron star PSR J0348[Formula: see text]0432 and its proto neutron star is studied in the framework of the relativistic mean field theory considering neutrino trapping. We see that the central baryon number density of the proto neutron star PSR J0348+0432 is in the range [Formula: see text][Formula: see text]fm[Formula: see text], which is smaller than that of the neutron star PSR J0348[Formula: see text]0432 [Formula: see text][Formula: see text]fm[Formula: see text]. Inside the neutron star PSR J0348[Formula: see text]0432, only the neutrons, protons, [Formula: see text] and [Formula: see text] produce, whereas the hyperons [Formula: see text] and [Formula: see text] all do not appear. But in the proto neutron star PSR J0348[Formula: see text]0432, hyperons [Formula: see text], [Formula: see text], [Formula: see text] and [Formula: see text] all will produce, though their relative particle number density is still very small, no more than 2%. This shows that higher temperature will be advantageous to the hyperon production.

RELATIVISTIC MEAN FIELD THEORETICAL FOUNDATION OF THE DROPLET MODEL FOR NUCLEI

2002 ◽  
Vol 11 (01) ◽  
pp. 55-65 ◽  
Author(s):  
CHUN-YUAN GAO ◽  
QI-REN ZHANG
Keyword(s):  
Mass Formula ◽  
Energy Surface ◽  
Theoretical Foundation ◽  
Mean Field Theory ◽  
Mean Field ◽  
Binding Energies ◽  
Droplet Model ◽  
Relativistic Mean Field ◽  
Theoretical Foundations ◽  
Type Mass

The binding energies per-nucleon for 1654 nuclei, whose mass numbers range from 16 to 263 and charge numbers range from 8 to 106, are calculated by the relativistic mean field theory, with finite nucleon size effect being taken into account. The calculated energy surface goes through the middle of experimental points, and the root mean square deviation for the binding energies per-nucleon is 0.08163 MeV. The numerical results may be well simulated by a droplet model type mass formula. The droplet model is therefore put on the relativistic mean field theoretical foundations.

Ground State Properties of Z = 114 Isotopes in the Relativistic Mean-Field Theory

1997 ◽  
Vol 14 (4) ◽  
pp. 259-262 ◽  
Author(s):  
Ren Zhong-zhou ◽  
Zhu Zhi-yuan ◽  
Cai Yan-huang ◽  
Shen Yao-song ◽  
Zhan Wen-long ◽  
...  
Keyword(s):  
Field Theory ◽  
Ground State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Relativistic Mean Field Theory ◽  
Relativistic Mean Field ◽  
Ground State Properties
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