Quark phases in neutron stars and a "third family" of compact stars as a signature for phase transitions

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dc.creatorSchertler, K.
dc.creatorGreiner, C.
dc.creatorSchaffner-Bielich, J.
dc.creatorThoma, M. H.
dc.date2000-01-26
dc.date.accessioned2026-07-07T11:33:59Z
dc.date.available2026-07-07T11:33:59Z
dc.descriptionThe appearance of quark phases in the dense interior of neutron stars provides one possibility to soften the equation of state (EOS) of neutron star matter at high densities. This softening leads to more compact equilibrium configurations of neutron stars compared to pure hadronic stars of the same mass. We investigate the question to which amount the compactness of a neutron star can be attributed to the presence of a quark phase. For this purpose we employ several hadronic EOS in the framework of the relativistic mean-field (RMF) model and an extended MIT bag model to describe the quark phase. We find that - almost independent of the model parameters - the radius of a pure hadronic neutron star gets typically reduced by 20-30% if a pure quark phase in the center of the star does exist. For some EOS we furthermore find the possibility of a "third family" of compact stars which may exist besides the two known families of white dwarfs and neutron stars. We show how an experimental proof of the existence of a third family by mass and radius measurements may provide a unique signature for a phase transition inside neutron stars.
dc.description37 pages, 18 eps-figures included, LaTeX
dc.identifierhttps://arxiv.org/abs/astro-ph/0001467
dc.identifierhttp://arxiv.org/abs/astro-ph/0001467
dc.identifierNucl.Phys.A677:463-490,2000
dc.identifierdoi:10.1016/S0375-9474(00)00305-5
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/198093
dc.subjectAstrophysics
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectNuclear Theory
dc.titleQuark phases in neutron stars and a "third family" of compact stars as a signature for phase transitions
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