Abstract
In this work, we discuss the deconfinement phase transition to quark matter in hot/dense matter. We examine the effect that different charge fractions, isospin fractions, net strangeness, and chemical equilibrium with respect to leptons have on the position of the coexistence line between different phases. In particular, we investigate how different sets of conditions that describe matter in neutron stars and their mergers, or matter created in heavy-ion collisions affect the position of the critical end point, namely where the first-order phase transition becomes a crossover. We also present an introduction to the topic of critical points, including a review of recent advances concerning QCD critical points.
Highlights
Introduction to Critical PointsIn thermodynamics, a critical point refers to the end point of a phase equilibrium curve
We have analyzed the differences that arise from the relaxation of the assumption of local conserved quantities, such as electric charge and lepton fraction, to global quantities [95]. Such relaxation widens the phase transition as a function of baryon chemical potential or free energy, there is no change in the position of the critical point
Since in this work we focus on the discussion of critical points, we assume that the surface tension of quark matter is very large, in which case mixtures of phases do not appear and ours constraints related to strangeness, charge, and isospin can be carried out locally
Summary
A critical point refers to the end point of a phase equilibrium curve. At zero baryon chemical potential, μ B = 0, baryons and antibaryons or quarks and antiquarks are in chemical equilibrium (with respect to the strong, not the weak force) with one another In this case, at finite temperature, it is possible to determine the QCD pressure and additional thermodynamic quantities numerically with controllable accuracy on the lattice. The significant rise in pressure with increasing temperature indicates the change in phase from a hadron gas to a quark-gluon plasma In particular, on how the end point of the first-order phase transition line changes for particular cases associated with different astrophysical and laboratory scenarios
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