Abstract
The effect of conserved baryon, isospin and strangeness charges on the behavior of phase transitions in dense matter is studied. Baryonic matter is described within the three-flavor Polyakov$-$Nambu$-$Jona-Lasinio model and several charge fractions $Y_Q$ are considered. The role of the vector interaction, which can be important to describe dense systems, is discussed. Special attention is given to the case with charge fraction $Y_Q=0.4$, due to its importance in heavy-ion collisions and core-collapse supernova matter. It is shown that the possible formation of chiral-symmetric quark matter in the laboratory will be favored in asymmetric matter. Besides, the inclusion of the vector interaction reinforces the formation of quark matter at lower densities.
Highlights
We investigate the phase transition associated with the restoration of chiral symmetry in a system with more than one conserved charge: baryonic charge, isospin, and strangeness
This is relevant for scenarios where asymmetric matter occurs, like in heavyion collisions (HICs) [1] and compact stars [2]
For more than one globally conserved charge, such as baryon, isospin, and/or strangeness, phase equilibrium has to be implemented by imposing Gibbs rules, which modify both the structure of the mixed phase and the determination of the transition point
Summary
We investigate the phase transition associated with the restoration of chiral symmetry in a system with more than one conserved charge (multicomponent systems): baryonic charge, isospin, and strangeness. This is relevant for scenarios where asymmetric matter occurs, like in heavyion collisions (HICs) [1] and compact stars [2]. For more than one globally conserved charge, such as baryon, isospin, and/or strangeness, phase equilibrium has to be implemented by imposing Gibbs rules, which modify both the structure of the mixed phase and the determination of the transition point. When only one globally conserved charge is allowed, the phase equilibrium is obtained by a Maxwell construction at constant pressure
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