scholarly journals A new equation of state Based on Nuclear Statistical Equilibrium for Core-Collapse Simulations

2011 ◽  
Vol 7 (S279) ◽  
pp. 333-334
Author(s):  
Shun Furusawa ◽  
Shoichi Yamada ◽  
Kohsuke Sumiyoshi ◽  
Hideyuki Suzuki
Keyword(s):  
Free Energy ◽  
Equation Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Statistical Equilibrium ◽  
Core Collapse ◽  
Average Mass ◽  
Relativistic Mean Field ◽  
Model Free ◽  
New Equation

AbstractWe calculate a new equation of state for baryons at sub-nuclear densities for the use in core-collapse simulations of massive stars. The formulation is the nuclear statistical equilibrium description and the liquid drop approximation of nuclei. The model free energy to minimize is calculated by relativistic mean field theory for nucleons and the mass formula for nuclei with atomic number up to ~ 1000. We have also taken into account the pasta phase. We find that the free energy and other thermodynamical quantities are not very different from those given in the standard EOSs that adopt the single nucleus approximation. On the other hand, the average mass is systematically different, which may have an important effect on the rates of electron captures and coherent neutrino scatterings on nuclei in supernova cores.

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

Covariant Equation of State for Two Colliding Nuclear Matters in the Relativistic Meson Field Theory

1997 ◽  
Vol 06 (01) ◽  
pp. 151-159 ◽  
Author(s):  
M. Rashdan
Keyword(s):  
Field Theory ◽  
Equation Of State ◽  
Nonlinear Models ◽  
Mean Field Theory ◽  
Mean Field ◽  
Heavy Ion ◽  
Ion Scattering ◽  
Relativistic Mean Field ◽  
Heavy Ion Scattering ◽  
Covariant Equation

The relativistic mean field theory (linear and nonlinear) models are extended to the case of two colliding nuclear matters, relevant to heavy ion scattering and reactions. The effect of vacuum corrections is taken into account through the relativistic Hartree approximation. The Fermi sea is assumed to consist of two colliding Lorentz elongated spheres. A relativistic covariant Pauli correction is considered for the overlap case. This relativistic Pauli correction is found to be very important due to its dependence on the effective nucleon mass which strongly depends on the model equation of state. It is found that by increasing the velocity the energy per baryon increases and saturates at higher densities. The increase in the energy per baryon at low density (the region of no overlap) is much larger than that at high density (the region of large overlap), due to Pauli correction effects. The saturation density of the nonlinear model is shifted to larger values than that of the linear model. Vacuum corrections effects are found to reduce largely te overlap region.

EFFECTS OF Δ-BARYON INTERACTION STRENGTH ON NEUTRON STARS PROPERTIES

2007 ◽  
Vol 16 (02n03) ◽  
pp. 175-183 ◽  
Author(s):  
J. C. T. DE OLIVEIRA ◽  
S. B. DUARTE ◽  
H. RODRIGUES ◽  
M. CHIAPPARINI ◽  
M. KYOTOKU
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Mean Field Theory ◽  
Mean Field ◽  
Interaction Strength ◽  
Hadronic Matter ◽  
Resonance Neutron ◽  
Baryon Interaction ◽  
Relativistic Mean Field ◽  
Central Regions

We investigate the effect of Δ-resonance interaction strength on the equation of state of asymmetric hadronic matter and neutron stars structure. We discuss Δ-matter formation at high densities in the context of a relativistic mean field theory. We show that the attractive nature of the Δ-baryon interaction can induce a phase transition accompanying Δ-matter formation, at values of densities presumably existing in central regions of neutron stars. The possibility of a rich Δ-resonance neutron star is presented using the proposed equation of state.

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.

RELATIVISTIC MEAN FIELD THEORY FOR UNSTABLE NUCLEI AND SUPERNOVAE

2003 ◽  
Vol 17 (28) ◽  
pp. 5175-5184
Author(s):  
HIROSHI TOKI
Keyword(s):  
Field Theory ◽  
Experimental Data ◽  
Equation Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Microscopic Theory ◽  
Phenomenological Theory ◽  
Relativistic Mean Field ◽  
Unstable Nuclei ◽  
Finite Nuclei

We discuss first the properties of unstable nuclei in the framework of the relativistic mean field (RMF) theory. We take the RMF theory as a phenomenological theory with several parameters, whose form is constrained by the successful microscopic theory (RBHF), and whose values are extracted from the experimental data of unstable nuclei. We find the outcome with the use of the parameter sets (TM1 and TMA) is promising in comparison with various experimental data on finite nuclei including unstable ones. We construct then the equation of state of nuclear matter for the use in the description of supernovae. We present also the simulations of supernovae with the supernova newly constructed equation of state in the prompt explosion scenario.

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.

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