Abstract
The microscopic composition and properties of matter at super-saturation densities have been the subject of intense investigation for decades. The scarcity of experimental and observational data has lead to the necessary reliance on theoretical models. However, there remains great uncertainty in these models, which, of necessity, have to go beyond the over-simple assumption that high density matter consists only of nucleons and leptons. Heavy strange baryons, mesons and quark matter in different forms and phases have to be included to fulfil basic requirements of fundamental laws of physics. In this review the latest developments in construction of the Equation of State (EoS) of high-density matter at zero and finite temperature assuming different composition of the matter are surveyed. Critical comparison of model EoS with available observational data on neutron stars, including gravitational masses, radii and cooling patterns is presented. The effect of changing rotational frequency on the composition of neutron stars during their lifetime is demonstrated. Compatibility of EoS of high-density, low temperature compact objects and low density, high temperature matter created in heavy-ion collisions is discussed.
Highlights
One of the central questions of current theoretical physics is what constitutes the structure of matter at high densities and temperatures
03009-p.2 (ii) Is the mean-field potential constrained enough by physical arguments ? Otherwise the results of fits of its parameters to the data may be correlated so that no uniques answer can be achieved. (iii) Is it justifiable to assume that the Equation of State (EoS) for a symmetric and pure neutron matter at zero temperature, extrapolated from the transport theory fitted to the Heavy-ion collisions (HI) collision process, can be applied to matter in cold neutron stars and core-collapse supernova with very different nature
Perhaps most interesting and relevant for this work is the evolution of the core-collapse supernova (CCS) core into a hot proto-neutron star and the eventual cooling to a stable cold neutron star
Summary
One of the central questions of current theoretical physics is what constitutes the structure of matter at high densities and temperatures. E/A is unknown and has to be determined from nuclear and/or particle physics models. Descriptions of quark matter range from different forms of the MIT bag, the Nambu-Jona-Lasinio, Chromo-Dielectric, DysonSchwinger models, as well as perturbative approach to QCD and implementation of the Polyakov-loop technique at non-zero temperature [9,10,11,12,13]. The EoS obviously varies in different temperature/energy density regimes which in turn dictate the most likely composition of the matter. Some other considerations, such as stability (equilibrum) of the matter must have to be taken into account.
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