scholarly journals QCD equation of state at finite chemical potentials for relativistic nuclear collisions

2021 ◽  
Vol 36 (07) ◽  
pp. 2130007
Author(s):  
Akihiko Monnai ◽  
Björn Schenke ◽  
Chun Shen
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Lattice Qcd ◽  
Baryon Number ◽  
Nuclear Collisions ◽  
Chemical Potentials ◽  
Dense Nuclear Matter ◽  
Lower Beam ◽  
Quantitative Understanding ◽  
Relativistic Nuclear Collisions

We review the equation of state of QCD matter at finite densities. We discuss the construction of the equation of state with net baryon number, electric charge, and strangeness using the results of lattice QCD simulations and hadron resonance gas models. Its application to the hydrodynamic analyses of relativistic nuclear collisions suggests that the interplay of multiple conserved charges is important in the quantitative understanding of the dense nuclear matter created at lower beam energies. Several different models of the QCD equation of state are discussed for comparison.

scholarly journals Constraining the equation of state of dense nuclear matter using thermal emission of neutron stars

2020 ◽  
Vol 1667 ◽  
pp. 012001
Author(s):  
Nicolas Baillot d’Étivaux ◽  
Jérôme Margueron ◽  
Sebastien Guillot ◽  
Natalie Webb ◽  
Màrcio Catelan ◽  
...  
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Thermal Emission ◽  
Dense Nuclear Matter

scholarly journals Nuclear equation of state and neutron star cooling

2017 ◽  
Vol 26 (04) ◽  
pp. 1750015 ◽  
Author(s):  
Yeunhwan Lim ◽  
Chang Ho Hyun ◽  
Chang-Hwan Lee
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Thermal Evolution ◽  
Observation Data ◽  
Nuclear Equation Of State ◽  
The Core ◽  
Dense Nuclear Matter ◽  
Nuclear Models

In this paper, we investigate the cooling of neutron stars with relativistic and nonrelativistic models of dense nuclear matter. We focus on the effects of uncertainties originated from the nuclear models, the composition of elements in the envelope region, and the formation of superfluidity in the core and the crust of neutron stars. Discovery of [Formula: see text] neutron stars PSR J1614−2230 and PSR J0343[Formula: see text]0432 has triggered the revival of stiff nuclear equation of state at high densities. In the meantime, observation of a neutron star in Cassiopeia A for more than 10 years has provided us with very accurate data for the thermal evolution of neutron stars. Both mass and temperature of neutron stars depend critically on the equation of state of nuclear matter, so we first search for nuclear models that satisfy the constraints from mass and temperature simultaneously within a reasonable range. With selected models, we explore the effects of element composition in the envelope region, and the existence of superfluidity in the core and the crust of neutron stars. Due to uncertainty in the composition of particles in the envelope region, we obtain a range of cooling curves that can cover substantial region of observation data.

Spikes in ring-type events from ultra relativistic nuclear collisions

2008 ◽  
Vol 86 (7) ◽  
pp. 919-922 ◽  
Author(s):  
D Ghosh ◽  
A Deb ◽  
M B Lahiri ◽  
A Bhattacharya
Keyword(s):  
Refractive Index ◽  
Nuclear Matter ◽  
Gluon Radiation ◽  
Ring Type ◽  
Nuclear Collisions ◽  
Nuclear Interactions ◽  
Relativistic Nuclear Collisions

This paper reports the observation of some peculiar ring-like events in ultra relativistic nuclear interactions (the 32S–AgBr interaction at 200 A GeV and the 16O–AgBr interaction at 60 A GeV). These events have been analysed in the light of Čerenkov gluon radiation as proposed by Dremin. Also the value of the refractive index of the nuclear matter is calculated. The analysis shows values of refractive index different from that revealed in normal nuclear matter. PACS Nos.: 25.75.–q, 24.60.Ky, 12.40.Ee

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

1988 ◽  
Vol 201 (1) ◽  
pp. 11-16 ◽  
Author(s):  
M. Cubero ◽  
M. Schönhofen ◽  
H. Feldmeier ◽  
W. Nörenberg
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Nuclear Equation Of State ◽  
Dense Nuclear Matter

ON A “MICROSCOPIC HUBBLE CONSTANT” FROM RELATIVISTIC NUCLEAR COLLISIONS

2007 ◽  
Vol 16 (07n08) ◽  
pp. 1790-1799 ◽  
Author(s):  
ALEXANDRU JIPA ◽  
CĂLIN BEŞLIU ◽  
ION SORIN ZGURĂ ◽  
OANA RISTEA ◽  
CĂTĂLIN RISTEA ◽  
...  
Keyword(s):  
Nuclear Matter ◽  
Temporal Evolution ◽  
Identical Particle ◽  
Hubble Constant ◽  
Big Bang ◽  
Nuclear Collisions ◽  
Particle Spectra ◽  
Relativistic Nuclear Collisions ◽  
The Universe ◽  
Universe Evolution

Similarities between cosmological scenarios on the Universe evolution after “Big Bang” and the behavior of the highly excited nuclear matter formed in relativistic nuclear collisions, immediately after collisions, are considered to do an estimation of a “microscopic Hubble parameter/constant” for the expansion rate in relativistic nuclear collisions, similar with the cosmological Hubble constant. Temporal connections between the evolution of the nuclear matter after impact and the scenarios on the Universe evolution after “Big Bang” are introduced. Experimental results on participants, fireball sizes (identical particle interferometry), densities, particle spectra and temperatures have been used. A “Hubble scale” for temporal evolution can be obtained. Satisfactory agreement with Buda-Lund model estimations has been obtained.

scholarly journals Thermal properties of hot and dense matter: Influence of rapid rotation on protoneutron stars, hot neutron stars, and neutron star merger remnants

2021 ◽  
Vol 252 ◽  
pp. 05004
Author(s):  
Polychronis Koliogiannis ◽  
Charalampos Moustakidis
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Equations Of State ◽  
Interaction Model ◽  
Dense Matter ◽  
Baryon Density ◽  
Dense Nuclear Matter ◽  
Protoneutron Stars

The knowledge of the equation of state is a key ingredient for many dynamical phenomena that depend sensitively on the hot and dense nuclear matter, such as the formation of protoneutron stars and hot neutron stars. In order to accurately describe them, we construct equations of state at FInite temperature and entropy per baryon for matter with varying proton fractions. This procedure is based on the momentum dependent interaction model and state-of-the-art microscopic data. In addition, we investigate the role of thermal and rotation effects on microscopic and macroscopic properties of neutron stars, including the mass and radius, the frequency, the Kerr parameter, the central baryon density, etc. The latter is also connected to the hot and rapidly rotating remnant after neutron star merger. The interplay between these quantities and data from late observations of neutron stars, both isolated and in matter of merging, could provide useful insight and robust constraints on the equation of state of nuclear matter.

Properties of cold dense nuclear matter based on a developed chiral perturbation theory

2015 ◽  
Vol 24 (08) ◽  
pp. 1550065
Author(s):  
Qingwu Wang ◽  
Xiaoya Li ◽  
Xiaofu Lü
Keyword(s):  
Perturbation Theory ◽  
Nuclear Matter ◽  
Chiral Perturbation Theory ◽  
Chemical Potential ◽  
Baryon Number ◽  
Number Density ◽  
Resonance Contribution ◽  
Chiral Perturbation ◽  
Dense Nuclear Matter ◽  
Natural Way

A developed effective chiral Lagrangian approach is used to study the cold dense nuclear matter. Improved calculation of baryon number density as a function of chemical potential is given. The resonance appeared in a natural way as chemical potential is getting larger. Calculations of susceptibility and pressure including the resonance contribution are also given.

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