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.

scholarly journals Isoscalar giant monopole resonance for drip-line and super heavy nuclei in the framework of relativistic mean field formalism with scaling calculation

Open Physics ◽  
2014 ◽  
Vol 12 (8) ◽  
Author(s):  
Subrata Biswal ◽  
Suresh Patra
Keyword(s):  
Excitation Energy ◽  
Mean Field Theory ◽  
Mean Field ◽  
Magic Numbers ◽  
Heavy Nuclei ◽  
Isotopic Chain ◽  
Excitation Energies ◽  
Relativistic Mean Field ◽  
Giant Monopole Resonance ◽  
Super Heavy Nuclei

AbstractWe study the isoscalar giant monopole resonance for drip-lines and super heavy nuclei in the framework of relativistic mean field theory with a scaling approach. The well known extended Thomas-Fermi approximation in the nonlinear σ-ω model is used to estimate the giant monopole excitation energy for some selected light spherical nuclei starting from the region of proton to neutron drip-lines. The application is extended to the super heavy region for Z=114 and 120, which are predicted by several models as the next proton magic numbers beyond Z=82. We compared the excitation energy obtained by four successful force parameters NL1, NL3, NL3*, and FSUGold. The monopole energy decreases toward the proton and neutron drip-lines in an isotopic chain for lighter mass nuclei, in contrast to a monotonic decrease for super heavy isotopes. The maximum and minimum monopole excitation energies are obtained for nuclei with minimum and maximum isospin in an isotopic chain, respectively.

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.

TEST OF NL-RA1 RELATIVISTIC EFFECTIVE INTERACTION FOR THE STRUCTURE OF DEFORMED AND SUPERHEAVY NUCLEI

2012 ◽  
Vol 21 (06) ◽  
pp. 1250055 ◽  
Author(s):  
M. RASHDAN
Keyword(s):  
Effective Interaction ◽  
Mean Field Theory ◽  
Mean Field ◽  
Superheavy Element ◽  
Decay Chain ◽  
Alpha Decay ◽  
Binding Energies ◽  
Superheavy Nuclei ◽  
Relativistic Mean Field ◽  
Relative Errors

The NL-RA1 effective interaction of the relativistic mean field theory is employed to study the structure of deformed and superheavy nuclei, using an axially deformed harmonic oscillator basis. It is found that a fair agreement with the experimental data is obtained for the binding energies (BE), deformation parameters and charge radii. Comparison with NL-Z2, NLSH and NL3 interactions show that NL-Z2 gives good binding but larger radii, while NL-SH gives good radii but larger binding. The NL-RA1 interaction is also tested for the new deformed superheavy element with Z≥98. Excellent agreement with the experimental binding is obtained, where the relative error in BEs of Cf, Fm, No, Rf, Sg and Ea (Z = 110) isotopes are found to be of the order ~0.1%. The NL3 predicted larger binding and larger relative errors ~0.2–0.5%. Furthermore, the experimental Q-values of the alpha-decay of the superheavy elements 270110, 288114 and 292116 are satisfactory reproduced by NL-RA1 interaction, where the agreement is much better than that predicted by the phenomenological mass FRDM model. Furthermore, the alpha-decay chain of element 294118 are also better reproduced by NL-RA1 interaction.

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 ENERGY SYSTEMATICS OF HEAVY NUCLEI — MEAN FIELD MODELS IN COMPARISON

2011 ◽  
Vol 20 (06) ◽  
pp. 1379-1390 ◽  
Author(s):  
P.-G. REINHARD ◽  
B. K. AGRAWAL
Keyword(s):  
Mean Field ◽  
Binding Energies ◽  
Superheavy Nuclei ◽  
Heavy Nuclei ◽  
Hartree Fock ◽  
Relativistic Mean Field ◽  
Mean Field Models ◽  
Opposite Trend ◽  
Super Heavy Nuclei ◽  
Rmf Model

We compare the systematics of binding energies computed within the standard and extended versions of the relativistic mean-field (RMF) model and the Skyrme–Hartree–Fock (SHF) model. The general trends for the binding energies for super-heavy nuclei are significantly different for these models. The SHF models tend to underbind the superheavy nuclei, while RMF models show just the opposite trend. The extended RMF model seems to provide remarkable improvements over the results obtained for the standard RMF model.

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