Metastable strange matter and compact quark stars

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dc.creatorMalheiro, M.
dc.creatorFiolhais, M.
dc.creatorTaurines, A. R.
dc.date2003-04-04
dc.date.accessioned2026-07-07T10:47:36Z
dc.date.available2026-07-07T10:47:36Z
dc.descriptionStrange quark matter in beta equilibrium at high densities is studied in a quark confinement model. Two equations of state are dynamically generated for the {\it same} set of model parameters used to describe the nucleon: one corresponds to a chiral restored phase with almost massless quarks and the other to a chiral broken phase. The chiral symmetric phase saturates at around five times the nuclear matter density. Using the equation of state for this phase, compact bare quark stars are obtained with radii and masses in the ranges $R\sim 5 - 8$ km and $M\sim M_\odot$. The energy per baryon number decreases very slowly from the center of the star to the periphery, remaining above the corresponding values for the iron or the nuclear matter, even at the edge. Our results point out that strange quark matter at very high densities may not be absolutely stable and the existence of an energy barrier between the two phases may prevent the compact quarks stars to decay to hybrid stars.
dc.descriptionto appear on J. Phys. G
dc.identifierhttps://arxiv.org/abs/astro-ph/0304096
dc.identifierhttp://arxiv.org/abs/astro-ph/0304096
dc.identifierJ.Phys.G29:1045-1052,2003
dc.identifierdoi:10.1088/0954-3899/29/6/307
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/183591
dc.subjectAstrophysics
dc.subjectNuclear Theory
dc.titleMetastable strange matter and compact quark stars
dc.typetext

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