The Deconfinement Phase Transition in Proto-Neutron-Star Matter

Understand

In this work, we study in detail the deconfinement phase transition that takes place in hot/dense nuclear matter in the context of neutron stars and proto-neutron stars (in which lepton fraction is fixed).

• The possibility of different mixtures of phases with different locally and globally conserved quantities is considered in each case.
• For this purpose, the Chiral Mean Field (CMF) model, an effective relativistic model that includes self-consistent chiral symmetry restoration and deconfinement to quark matter, is employed.
• Finally, we compare our results with data provided by PQCD for different temperatures and conditions.