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Finite temperature quark matter and supernova explosion

Alessandro Drago and Ubaldo Tambini

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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.


PACS

97.60.Bw Supernovae

95.30.Cq Elementary particle processes

97.10.Cv Stellar structure, interiors, evolution, nucleosynthesis, ages

97.60.Jd Neutron stars

12.38.Aw General properties of QCD (dynamics, confinement, etc.)

11.10.Wx Finite-temperature field theory

Subjects

Particle physics and field theory

Astrophysics and astroparticles

Dates

Issue 5 (May 1999)

Received 21 September 1998, in final form 30 November 1998



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