Equation of state for aluminum in warm dense matter regime

A semi-empirical equation of state model for aluminum in a warm dense matter regime is constructed. The equation of state, which is subdivided into a cold term, thermal contributions of ions and electrons, covers a broad range of phase diagram from solid state to plasma state. The cold term and thermal contribution of ions are from the Bushman–Lomonosov model, in which several undetermined parameters are fitted based on equation of state theories and specific experimental data. The Thomas–Fermi–Kirzhnits model is employed to estimate the thermal contribution of electrons. Some practical modifications are introduced to the Thomas–Fermi–Kirzhnits model to improve the prediction of the equation of state model. Theoretical calculation of thermodynamic parameters, including phase diagram, curves of isothermal compression at ambient temperature, melting, and Hugoniot, are analyzed and compared with relevant experimental data and other theoretical evaluations.     

D-mesons in dense nuclear matter

The D-meson properties in dense nuclear matter are studied. The D-meson spectral density is obtained within the framework of a coupled-channel self-consistent calculation, assuming as bare meson-baryon interaction a separable potential. The resonance is generated dynamically in our coupled-channel model. The medium modifications of the D-meson properties due to Pauli blocking and the dressing of D-mesons, nucleons and pions are also studied. We conclude that the self-consistent coupled-channel process reduces the in-medium effects on the D-meson compared to previous literature which did not consider the coupled-channel structure.Received: 14 January 2005, Published online: 31 May 2005PACS: 14.40.Lb, 14.20.Gk, 21.65. + f     

Superfluidity in dense nuclear matter

We discuss the onset of superfluidity in neutron stars, where the model of nuclear matter is realized in a high-density and asymmetry state. In particular, we present the study of the effects of microscopic three-body forces on the proton pairing in the ¹ S ₀ channel and neutron pairing in ³ PF ₁ channel for β-stable neutron star matter. It is found that the main effects of three-body forces are to shrink the domain of existence of the ¹ S ₀ below the threshold of the direct URCA process and to stretch the density range of the ³ PF ₁ pairing in a broad domain so to cover most part of the neutron-star core. The text was submitted by the authors in English.     

Delta and pion abundances in hot dense nuclear matter and the nuclear equation of state

Delta and pion abundances in hot dense nuclear matter are calculated self-consistently within a relativistic mean-field model for different equations of state. The density of deltas turns out to be much more sensitive to the effective masses of the baryons than to the stiffness of the equation of state. The results are compared to experimental pion yields from intermediate-energy nucleus-nucleus collisions. The influence of deviations from thermal momentum distributions for the baryons is estimated.     

Equation of state of asymmetric nuclear matter: a VMC study

A Variational Monte Carlo (VMC) method is employed to investigate the properties of symmetric and asymmetric nuclear matter. The realistic Urbana V ₁₄ twonucleon interaction potential of Lagaris and Pandharipande was used to describe the microscopic interactions. Also, many body interactions are included as a density dependent term in the potential. Total kinetic and potential energies per particle are calculated for asymmetric nuclear matter by VMC method at various densities and isospin asymmetry parameters. The results are compared with data found in literature, and it was observed that the results obtained in this study reasonably agree with the results found in the literature. Also, the symmetry energy and incompressibility factor of the nuclear matter were obtained. The results obtained are in good agreement with those obtained by various authors with different methods and techniques.     

Strange mesons in dense nuclear matter

Experimental data on the production of kaons and antikaons in heavy-ion collisions at relativistic energies are presented and discussed with respect to in-medium effects. The K ^?/K⁺ ratios measured in nucleus-nucleus collisions are 1–2 orders of magnitude larger than in proton-proton collisions. The azimuthal angle distributions of K ⁺ mesons indicate a repulsive kaon-nucleon potential. Microscopic transport calculations consistently explain both the yields and the emission patterns of kaons and antikaons when assuming that their properties are modified in dense nuclear matter. The K ⁺ production excitation functions measured in light and heavy collision systems provide evidence for a soft nuclear equation-of-state.     

Exotica in dense and cold nuclear matter

A method for creating and investigating, under laboratory conditions, droplets of superdense cold matter is proposed, neutron stars being the closest analog of this kind of matter in nature. Arguments in support of the statement that an implementation of respective experiments is possible are presented, and the mechanism of kinematical cooling of the droplets in question is clarified. Various trigger types are proposed for performing searches for various exotic multiquark states in cold superdense matter.     

Equation of state of superdense matter

The possibility of the existence of anomalous nuclei in superdense stars as well as the possibility of the spontaneous transition of a superdense object as a whole into an anomalous state which can be due either to the Migdal or the Lee mechanisms are discussed. An equation of state is obtained for _Nucl by using data on the total proton-proton scattering cross section in the high-energy range.Translated from Izvestiya Vysshikh Uchbenykh Zavedenii, Fizika, No. 11, pp. 20–23, November, 1978.     

Equation of state for hadronic matter

An exact equation of state for a relativistic quantum gas model of hadronic matter is derived using analytical methods. Our results are shown to be an extension of the quantum gases through the inclusion of the hadronic mass spectrum ?(m).     

The strangeness and charm of dense nuclear matter

Acta Physica Hungarica A) Heavy Ion Physics - The creation of strangeness and charm in nucleus-nucleus collisions at threshold beam energies is discussed as a probe for compressed baryonic matter....     

Equation of state of asymmetric nuclear matter and the tidal deformability of neutron star

The European Physical Journal A - In recent years there has been much progress on the investigation of the QCD phase diagram with lattice QCD simulations. In this review we focus on the...     

Equation of state of zero-temperature quark matter

We outline the key elements of a recent calculation aimed at determining the equation of state of deconfined (but unpaired) quark matter at zero temperature and high density, using finite quark masses. The computation is performed in perturbation theory up to three loops, and necessitates the development and application of some novel computational tools. In this talk, we introduce the basic features of these new techniques and review the main sources of motivation for considering finite mass effects in perturbation theory.     

Ground state properties of nuclear matter

The ground state properties of nuclear matter are calculated in theΛ ₁₁-approximation¹. A nucleon-nucleon interaction of the Yamaguchi-type and thes-wave part ofTabakin's potential have been considered. In both cases too large values for the density of nuclear matter and the binding energy per nucleon are found. The momentum distribution turns out to be very small for momenta larger than the Fermi momentum.     

Equation of state of nuclear matter and neutron stars in a hadron mass scaling frame

The equation of state for nuclear matter at finite temperature and the properties of neutron stars are studied starting from an effective Lagrangian in the framework of the relativistic mean field theory. We find that the empirical properties of nuclear matter can be reproduced if the medium effects are mainly described in terms of the Brown-Rho mass scaling on top of the Bonn potential used as the underlying bare nucleon-nucleon interaction. In particular a correct symmetry energy at saturation density is obtained. The extrapolation of the equation of state to neutron matter and some predictions for the neutron-star masses are finally discussed and compared with other nucleonic many-body approaches.PACS: 21.65. + f Nuclear matter - 21.30.Fe Forces in hadronic systems and effective interactions - 97.60.Jd Neutron stars