Abstract
We study the equation of state (EOS) of quark matter at finite temperature, using a confinement model in which chiral symmetry remains broken in the deconfined phase. Using the Walecka model to describe the hadronic phase, a deconfinement transition at densities slightly larger than nuclear matter saturation density takes place in pre-supernova matter. The presence of a mixed-phase region softens the EOS and open the possibility of a direct explosion. At larger densities the EOS is stiff enough to support a neutron star compatible with observations.
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