scholarly journals QUARK/HADRONIC MATTER AND DUALITIES OF QCD THERMODYNAMICS

2021 ◽  
Author(s):  
T. G. Khunjua ◽  
K. G. Klimenko ◽  
R. N. Zhokhov
Keyword(s):  
Hadronic Matter

scholarly journals Non-perturbative quarkonium dissociation in hadronic matter

1995 ◽  
Vol 356 (2-3) ◽  
pp. 349-353 ◽  
Author(s):  
D. Kharzeev ◽  
L. McLerran ◽  
H. Satz
Keyword(s):  
Hadronic Matter

Leading particle and nuclear-mass effects on multiparticle production in 50 GeV/c π− interactions in nuclear emulsion

1981 ◽  
Vol 59 (6) ◽  
pp. 812-819 ◽  
Author(s):  
S. C. Varma ◽  
V. Kumar ◽  
A. P. Sharma
Keyword(s):  
Magnetic Field ◽  
Experimental Study ◽  
Nuclear Emulsion ◽  
Hadronic Matter ◽  
Multiparticle Production ◽  
Particle Multiplicity ◽  
Nuclear Mass ◽  
Space Time Structure ◽  
Leading Particle ◽  
Grey Particle

An experimental study is carried out on the effects of nuclear mass on leading particle multiplicity and multiparticle production with the help of an emulsion stack exposed to 50 GeV/c π− beam under a strong pulsed magnetic field. The study of the effect of nuclear mass on the forward–backward asymmetry in a π−–A collision is also carried out using the grey particle multiplicity data. The results support the concept of "formation length" of radiation. An attempt is made to explain the space–time structure of hadronic matter in terms of the additive quark model of multiparticle production.

scholarly journals Speed of sound in hadronic matter using non-extensive Tsallis statistics

2016 ◽  
Vol 52 (9) ◽  
Author(s):  
Arvind Khuntia ◽  
Pragati Sahoo ◽  
Prakhar Garg ◽  
Raghunath Sahoo ◽  
Jean Cleymans
Keyword(s):  
Speed Of Sound ◽  
Hadronic Matter ◽  
Tsallis Statistics

Microcosmos and Macrocosmos: A Look at these Two Universes in a Unified Way

1997 ◽  
Vol 12 (07) ◽  
pp. 1373-1384 ◽  
Author(s):  
P. R. Silva
Keyword(s):  
Strong Interaction ◽  
Gravitational Force ◽  
Inertial Mass ◽  
Hadronic Matter ◽  
Vacuum Pressure ◽  
Bag Model ◽  
Small Oscillations ◽  
Mit Bag Model ◽  
Two Universes ◽  
The Universe

An extension of the MIT bag model, developed to describe the strong interaction inside the hadronic matter (nucleons), is proposed as a means to account for the confinement of matter in the universe. The basic hypotheses of the MIT bag model are worked out in a very simplified way and are also translated in terms of the gravitational force. We call the nucleon "microcosmos" and the bag-universe "macrocosmos." We have found a vacuum pressure of 10-15 atm at the boundary of the bag-universe as compared with a pressure of 1029 atm at the boundary of the nucleon. Both universes are also analyzed in the light of Sciama's theory of inertia, which links the inertial mass of a body to its interaction with the rest of the universe. One of the consequences of this work is that the Weinberg mass can be interpreted as a threshold mass, namely the mass where the frequency of the small oscillations of a particle coupled to the universe matches its de Broglie frequency. Finally, we estimate an averaged density of matter in the universe, corresponding to [Formula: see text] of the critical or closure density.

QUARK MATTER NUCLEATION IN NEUTRON STARS

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1491-1498 ◽  
Author(s):  
I. BOMBACI
Keyword(s):  
Phase Transition ◽  
Critical Mass ◽  
Threshold Value ◽  
Hadronic Matter ◽  
First Order Phase Transition ◽  
Nucleation Mechanisms ◽  
Deconfinement Phase Transition ◽  
Quark Deconfinement ◽  
Evolutionary Paths ◽  
First Order Phase

We study the quark deconfinement phase transition in cold (T = 0) and hot β-stable hadronic matter. Assuming a first-order phase transition, we calculate and compare the nucleation rate and the nucleation time due to thermal and quantum nucleation mechanisms. We show that above a threshold value of the central pressure a pure hadronic star (HS) is metastable to the conversion to a quark star (QS) (i.e. hybrid star or strange star). We introduce the concept of critical mass M cr for cold HSs and proto-hadronic stars, and the concept of limiting conversion temperature for proto-hadronic stars. We show that proto-hadronic stars with a mass M < M cr could survive the early stages of their evolution without decaying to QSs. Finally, we discuss the possible evolutionary paths of proto-hadronic stars.

scholarly journals Chiral Lagrangian for strange hadronic matter

1998 ◽  
Vol 57 (5) ◽  
pp. 2576-2588 ◽  
Author(s):  
P. Papazoglou ◽  
S. Schramm ◽  
J. Schaffner-Bielich ◽  
H. Stöcker ◽  
W. Greiner
Keyword(s):  
Hadronic Matter ◽  
Chiral Lagrangian

Quark Clustering and Chiral Symmetry Breaking in Nuclear Matter

2003 ◽  
Vol 18 (32) ◽  
pp. 2255-2264 ◽  
Author(s):  
O. A. Battistel ◽  
G. Krein
Keyword(s):  
Symmetry Breaking ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Chiral Symmetry ◽  
Quark Matter ◽  
Traditional Approach ◽  
Chiral Symmetry Breaking ◽  
Quark Condensate ◽  
Baryon Density ◽  
Hadronic Matter

Chiral symmetry breaking at finite baryon density is usually discussed in the context of quark matter, i.e. a system of deconfined quarks. Many systems like stable nuclei and neutron stars however have quarks confined within nucleons. In this paper we construct a Fermi sea of three-quark nucleon clusters and investigate the change of the quark condensate as a function of baryon density. We study the effect of quark clustering on the in-medium quark condensate and compare results with the traditional approach of modeling hadronic matter in terms of a Fermi sea of deconfined quarks.

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